Download - Abstract Book [PDF, 2.1MB]
w w w . a s t r o . g l a . a c . u k / n a m 2 0 1 0
A B
S T
R A
C T
S
The NAM Local Organising Committee would like to thank the following organisations for their generous support of
NAM 2010
National Astronomy Meeting
Abstracts Book
2010 April 12–16
http://www.astro.gla.ac.uk/nam2010/
National Astronomy Meeting
Abstracts Book
2010 April 12–16
ContentsWelcome! 2
Acknowledgements 4SocialEvents 5
Outreachevents 6Localinformation 7
Sessions 14RAS Afternoon 40
Abstracts 42IndexofAuthors 91
Listofparticipants 97
Wel
com
e! AndyFabian
As President of the Royal AstronomicalSociety(RAS),itgivesmegreatpleasuretowelcomeyoutoGlasgowUniversityforthe2010RAS NationalAstronomyMeet-ing, the UK’s largest annual astronomyandspacescienceevent. Morethan500scientists are registered for theMeeting,frompostgraduate students to senior re-searchersandacademicstaff. Duringtheweek, wewilldiscussandpresentcutting-edgesciencefromacrossourfield, fromthe upper atmosphere of the Earth togalaxiesintheearlyUniverse. IntheUKwearenotonlyoutstandinginourfield,rankingsecondto theUS,butoutstand-ingatcommunicatingourwork. Astron-omy’sprofileinthemediaishigherthanever, hasanenduringpopularitywithstudents inour schoolsand iscitedbymanyasakeyfactorforinspiringentryintoacareerinscience. SoatNAM2010wecancelebratethebestofourscienceinaninstitutionwhereastronomyhasbeentaughtforhalfamillennium, andresearchedindepthsincethe1760ap-pointmentofAlexanderWilsonas thefirstRegiusChairofAstronomy, rightlycelebratedinthis250thanniversaryyear. Glasgowisagreatplaceforouran-nualMeetingtotakeplaceandwhateveryourareaofworkI hopetoseeandtalktomanyofyouinthedaysahead.
AndyFabian, PresidentoftheRoyalAstronomicalSociety
JohnC Brown
OnbehalfoftheLOC,SOC andalllocalGlasgow area astronomers, professionalandamateur, I extend toallNAM 2010delegates a verywarmwelcome to ourfinecityandtotheGU CampusNAM site.WealsowishtothankRAS/NAM forac-ceptingourinvitationtothissiteinrecog-nition of the 250th Anniversary of ourRegiusChairofAstronomy. Solarphysics,MIST andAstronomyhaveundergonead-vancesunimaginableinWilson’sdayandastonishingeven since the lastGlasgowNAM (thenanRAS OutofTownMeeting)in1989. Enjoyallthelatestsciencenewsherebut alsomake sure you take sometimetoenjoyourcity, environs, andleg-endaryhospitality
JohnC Brown, 10thRegiusChairofAs-tronomyand10thAstronomerRoyal forScotland
250yearsoftheRegiusChairofAstronomyinGlasgow: AlexanderWilson, firstRegiusChair
Alexander Wilson MA, MD was thefirstappointee(1760-1784)totheRegiusChairofPracticalAstronomy, Universityof Glasgow (founded 1451). This fol-lowedestablishmentofthefirstdedicatedUniversity Observatory in 1757, basedon an instrument collection donated byAlexander McFarlane of Jamaica. Re-furbishmentoftheinstrumentsaftertheirdeleterious voyagewere carried out for£5byJamesWatt, atthattimea19yearoldUniversity instrumentmaker. TherehavebeentenRegiusChairstodate, thecurrentincumbent, JohnC Brown, beingalso10thAstronomerRoyalforScotland.
Born in St Andrews, Wilson graduatedMA (1733)thereandbecameanappren-ticetoaLondonsurgeonandapothecary. HereturnedtoStAndrewsin1739tostarta type foundrybusinesswhichmoved toGlasgowin1744, supplyingtheUniversity printers. In business partnershipwith JamesWatt and JosephBlack, hemade some of the earliest scientific thermometerswhich played acentralroleinBlack’sworkontheoriesoflatentandspecificheat. PriortohisChair appointment, Wilsonhad invented a newprocess for type, made tele-scopes, flownthermometersonkites, andmadespecificgravitybeadsforliq-uid testing includingspirit ‘proof’ strength. WhileRegiusChairhewasClerkofSenateand foundermemberof theRoyalSocietyofEdinburgh, aswellasbeing very active in several areas of research, most famously for his obser-vational discovery [Philosophical Transactions (1683–1775), 64:1–30 (1774),doi:10.1098/rstl.1774.0001, ADS:1774RSPT...64....1W] oftheapparentdepres-sionofsunspotsbelowthephotosphere, todaytermedtheWilsonEffect.
[ImageofWilsoncourtesyof JamesBabingtonSmith, Wilsondescendant; ex-cerptsofWilsonpapercourtesyoftheRoyalSociety]
3
Ack
now
ledg
emen
ts The LocalOrganising Committee Lyndsay Fletcher (LOC chair), John Brown(LOC DeputyChair), RachaelMcLauchlan(Secretary), MatthewCartmell(De-partmentofMechanicalEngineering), SaraDiegoli(ScottishUniversitiesPhysicsAlliance), DeclanDiver, HelenFraser(UniversityofStrathclyde), NormanGray,GilesHammond, IainHannah, IkSiongHeng, NicLabrosse, AlecMacKinnon(DepartmentofAdultandContinuingEducation), PeterMurray, MattPitkin, Bon-nieSteves(GlasgowCaledonianUniversity), GrahamWoan.
TheScientificOrganisingCommittee MartinHendry(SOC Chair), JohnBrown,EduardKontar(UKSP SOC chair), AnnetteFerguson(ROE IfA,UniversityofEdin-burgh), WayneHolland(UKATC,UniversityofEdinburgh), AndyTaylor(ROE IfA,UniversityofEdinburgh), AlanThompson(BGS Edinburgh, MIST SOC chair), IanBonnell(UniversityofSt. Andrews), JaneGreaves(UniversityofSt. Andrews),SheilaRowan(UniversityofGlasgow).
TheUKSP SOC GerryDoyle (Armagh), Rekha Jain (Sheffield,) EduardKontar(Glasgow; chair), DuncanMacKay(StAndrews), DavidPontin(Dundee).
TheMIST Council
Allofthe sessionconvenors forputtingtogethersuchanexcellentscientificpro-gramme.
OurteamofNAM helpers MattAbernathy, MarinaBattaglia, RiccardoBassiri,Euan Bennet, Nicola Beveridge, Christina Burge, Paul Campsie, EwanDick-son, MattEdgar, HodaGhodsi, ColinGill, DavidGraham, JingnanGuo, KarenHaughian, ErinMacdonald, ProchetaMallik, HeatherRatcliffe, HamishReid,SatoruSakai, IgnacioSantiago, EdwardThomson, FraserWatson.
JohnBrown, LucieGreen, ChrisLintott, FionaSpeirits, FredWatson, and JimWildasoutreacheventpresenters.
FredWatson, MarnieOgg, TheGlasgowSkepticsandTheAdmiralBar(‘ScienceinthePub’).
Alltheschoolswhoparticipatedintheschools’postersession.
Wewouldalsoliketothankthefollowinginthe UniversityofGlasgow fortheirhelpandadvice: IshbelDuncanandLucindaHay(TheConferenceandVisitorServicesOffice), ChaHannawayandBillYoung (AV and IT), EllenThompson(HospitalityServices), PatrickNwaozuzu(FInanceandPurchasingOffice), Stu-artForsyth (CorporateCommunications), AnnePlissiand JacquelineHeuchan(PhysicsandAstronomyAccountsOffice), AlanBowman(PhysicsandAstron-omyStores).
ThankstoIainHannahfortheimageoftheGlasgowUniversityCloistersusedonourAbstractBookandbanners.
Social Events
Monday12thApril
Reception: GlasgowCityChambers ThemeetingreceptionwillbehostedbyGlasgowCityCouncil in theCityChambers, situated in theheart of the citycentre. Thisreceptionincludesdrinksandcanapés. Advancedreservationwasrequired: youwillneedtoshowyourconferencebadgetoenter.
Thisisexpectedtorunfrom18.30to20.00.
ScienceinthePub: TheAdmiralBar A “ScienceinthePub”Q&A panelses-sion, ledbyFredWatsonofAAO,isplannedforMonday12thfrom20.30–23.00directlyaftertheCivicReception. FredWatsonmakesfrequentappearancesonAustralian radio andTV,which, togetherwithhis books, public lectures andastronomytourismexpeditions, haveresultedinseveralawards.
ThevenuewillbetheTheAdmiralBarintheCityCentre, abouta10/15minwalkfromtheCityChambers(Googledirections). ThevenueisaregularhauntofGlasgowSkepticsinthePubwhoarekindlyassistingwiththatevent. Advancedregistrationwasrequired, andalightbuffetwillbeprovidedforthosewhodidregister: showyourconferencebadgetoenter.
Tuesday13thApril
5-a-sideFootball: KelvinhallInternationalSportsArena Thisyear’scompetitionwilloccurindoorsinasportingvenuethathasheldmanyaninternationalsport-ingevent, theKelvinhall, justafewmomentswalkfromtheUniversity.
Thecompetitionisexpectedtorunfrom18.30to21.00.
Wednesday14thApril
Dinner&Ceilidh: KelvingroveArtGalleryandMuseum ThemeetingdinnerwillbefollowedbyatraditionalceilidhbothinthespectacularKelvingroveArtgalleryandMuseum, situatedjustdownthehillfromtheUniversity.
Pleasebringyourconferencebadge, whichalsoshowsthemenuchoiceswhichyoumadeatregistration.
Thedinnerisexpectedtorunfrom19.00to24.00.
Hubble3D previewatGlasgowScienceCentreIMAX
TheGlasgowScienceCentreisshowingthenewHubble3D IMAX film, andtheirprevieweventhasfallenonthe14th. Theyhavekindlyoffered100ticketsforNAMdelegates, soifyouareunabletogototheconferencedinner, thisisanotheralternative. Email SharonLyons ([email protected]) assoonaspossible, ifyouwanttobookaticket.
Youcanfindamapoftheselocationsat http://bit.ly/9v6jsq
Allweek
While inGlasgowmake sure tovisit theGlasgowScienceCentre, whohavespecialratesforNAM delegates. Seepage 9 fordetails.
Out
reac
h ev
ents Publicastronomytalks
Thesetalksarefreetoattend, butifyouhavenotalreadydoneso, pleasereserveafreee-ticketontheweb, at http://www.astro.gla.ac.uk/nam2010/pub.php. Allthetalkswilltakeplaceat19.30inlecturetheatre 257oftheKelvinBuilding,DepartmentofPhysicsandAstronomy, oncampusnexttothemainUniversitybuilding.
19:30Tuesday13thApril2010: TheMagicoftheSunandStars
JohnBrown (UniversityofGlasgow, andAstronomerRoyalforScotland) &LucieGreen (MullardSpaceScienceLaboratory). ExplorethewondersofourownSunandcountlessotherstarsthroughouttheuniverse.
19:30Wednesday14thApril2010: HowtoUseaMillionAstronomers–TheGalaxyZooandBeyond
ChrisLintott (UniversityofOxfordand“TheSkyatNight”). Discoverhow“Cit-izenScientists”arehelpingtounravelthemysteriesofhowgalaxiesformed.
19:30Thursday15thApril2010: HereistheSpaceWeather
JimWild (LancasterUniversity). Learnaboutthespaceenvironmentandhowits“weather”impactsonhumantechnology. InassociationwiththeAstronomicalSocietyofGlasgow, http://www.theasg.org.uk/
JohnBrown&LucieGreen ChrisLintott JimWild
250yearsoftheAstronomyChairatGlasgow
TheHunterianMuseum, nexttothePlenarysessions, willbehostingadisplayonAlexanderWilson. ThereisalsothechanceforasmallnumberofinteresteddelegatestoviewrelatedhistoricalmaterialsfromtheUniversityLibrary’sSpecialCollection(Wednesday14thatlunchtimeandintheafternoon–signupattheregistrationdesk).
Outreach
FridayoftheNAM willincludeaspecialschoolspostersession, from12.00to14.00in theKelvinBuilding(DepartmentofPhysicsandAstronomy). Duringtheweeksprior to themeeting, schoolpupils from thecouncilareasofWestDunbartonshire and South Lanarkshire havebeen researching sunspots, solaractivityandthepressingquestionofanylinkbetweentheseandterrestrialclimate–onethatwouldhaveinterestedAlexanderWilsonhimself. Inthispostersessiontheywillpresenttheirresults. Wehopethatmanyconferenceattendeeswilltaketheopportunitytopopinanddiscusstheireffortsandconclusionswiththem.
Local information
For a link-rich version of this information, see http://www.astro.gla.ac.uk/nam2010/out.php
ThereisahugenumberofplacesinGlasgowtoshop, visit, eat, drink, and/ordance. Sothefollowinglistisbynomeanscomprehensive, butpointstodifferentareasofinterestandwhatyoushouldfindthere.
TheWestEnd(G12)
ByresRoad isthemainstreetforshops, banks, restaurants, barsandpubsintheWestEndandis justa fewminuteswalkwestonUniversityAvenuefromthemainbuildingandNAM2010. ItalsocontainstheHillheadsubwaystop.
Subway HillheadShops Waitrose, Tesco, M&S SimplyFood, Iceland, Peckham’s, ClintonCards,
Clarks, Fopp, Superdrug, Specsavers, PapyrusPharmacy Boots
Banks/BuildingSocities RBS,HBOS,LloydsTSB,Clydesdale, Nationwide, San-tander
Take-a-away UniversityCafe, Starbucks, Subway, LittleItaly, Peckham’s, Gregg’s,HeartBuchanan, BaguetteExpress
Restaurants Paperino’s, OranMor, Balbir’s, Stravaign, theBothy, theTwoFigsPubs/Bars Tennents, OranMor, Aragon, CommonRoom
AshtonLane/CresswellLane isacobbledlanelinedbybarsandrestaurantsthatrunsparalleltoByresRoad, behindHillheadunderground.
Cinema GrosvenorFood&Drink UbiquitousChip(andthePubupstairs), Brel, theLoft, CafeAn-
daluzandmanymore
GreatWesternRoad isatthetopofByresRdandheadseastwardsintothectycentre(withvariousshopsandpubs)andwestwardintotheA82andthehigh-lands. AtthecornerofByresRdandGreatWesternRdistheBotanicGardenswithfreeentrytotherestoredKibblePalaceglasshouse.
Subway KelvinbridgeRestaurants CailBruichWest, TheBigBlue, Gambrino, WudonPubs/Bars OranMor, Coopers, TheBelle, TheWiseMonkey
WoodlandsRdandGibsonSt leadingoffoftheeastofUnivesityAvenue)featuresmoreplacestoeatanddrink.
ComedyClub TheStandPubs/Bars UisgeBeathe, DoubletBar, ThePrimaryRestaurants TheLeftBank, ChilliesWestEnd, TattieMac’s(OtagoSt)
DumbartonRd/SauchiehallSt/ArgyleSt(G3)
DumbartonRd isatthebottomofByresRd. GoingeastwarditsplitsintoArgyleStandSauchiehallStattheKelvingroveArtGallery. BothofthesestreetsendupbeingtwoofthemainshoppingstreetsintheCityCentre.
KelvingroveArtGalleriesandMuseum iscompletely free andawanderaboutisstrongly recommended. ItisthemostpopularfreevisitorattractioninScotlandandmostvisitedUK museumoutsideLondon. Ithasavarietyofexhibits(includ-ingtheobligatorydinosaurs, egyptiansarcophagi, armourandCharlesRennieMackintosh)andfamouspaintingsfromartistsincludingRembrandt, Matisse, Pi-casso, Monet, vanGogh, andparticularlySalvadorDali'sfamousChristofSaintJohnoftheCross. Andofcoursetheconferencedinnerandceilidhwillbethere.
MuseumofTransport isalso free. Itwillbeclosingforever(movingtoanewClydesidemuseumin2011)onthe19thofApril, sothereisaseriesofeventstakingplaceduringtheweekofNAM2010. Withtrams, trainsandships, thisplaceisabigkid’sdelight.
Subway Kelvinhall, PartickFood&Drinks TheGoat, BigSlope, TheSisters, Mother India (+Cafe), Fanny
Trollope’sPubs TheThreeJudges, Lismore, BenNevis
CityCentre
ThemainshoppingstreetinGlasgowareBuchananSt, SauchiehallSt(atthetopofBuchananSt)andArgyleSt(atthebottomofBuchananSt).
Thereisaconcentrationofpubsandrestaurantsinthe MerchantCity, particu-larlyMerchantSquare/Candleriggs (afewblocksoutheastofthecitychambers)
8
Subway BuchananSt, StEnochFood&Drinks TheButterfly&thePig, TwoFatLadies, 13thNote(Veggie), Stereo,
Rumours, TheDhabba, OkoExpress,Pubs the(legendary)HorseshoeBar, theLab, CountingHouse(bigWetherspoon’s
acrossfromcitychambers), O’Henry’s
Other
GlasgowScienceCentre/Hubble3D IMAXWhilstinGlasgow, makesuretovisitthe GlasgowScienceCentre (GSC),currentlyhometotheIYA’s‘ExplorersoftheUniverse’photographicexhibition, averyfineplanetarium, andahugeIMAXscreenshowingtheamazingIMAX 3D film‘Hubble’(thisstartsonApril15th,andyoucanbookfreeticketsforapreviewonthe14th–seepage 5 fordetails).TheScienceCentreisalsohostinganamazingexhibition‘WallaceandGromitpresentaWorldofCracking Ideas’whichexplores themesof innovationandinventionaswellasofferingaglimpseintoWallace’szanycreativeworld. AsadelegatetoNAM youwillbenefitfromaspecialdelegaterateof£4perpersonforadmissiontothemainScienceMallonproductionofyourdelegatebadgeattheScienceCentreticketdesk.
TheGSC islocatedonthesouthsideoftheClyde, 40minuteswalkfromthecampus, ortakeataxitotheCrownePlazahotelbytheSECC,andwalkacrossoneofthepedestrianbridges.
Balloch/LochLomond&theHighlands Balloch, thetownatthesouthernedgeofLochLomond, islessthananhourawaybytrainfromQueenStlowlevelrailstation, whichyoucanreachfromPartickstation. TofullyexploreLochLomondandthespectacularhighlandswerecommendacar. GreatWesternRoad, atthetopofByresRoadistheA82andthisoneroadtakesyoutoLochLomond, upbyRannochMoor, Glencoe(under2hoursdriveaway)thenontoFortWilliam,LochNessandeventuallyInverness(about4hoursdrive).
CarRental: Therearenocarhirelocationsconvenientfortheuniversity. Eithergetthecarattheairport(GlasgoworPrestwick)ortheEnterprise(40OswaldSt,G14PL) nexttoCentralstationinthecitycentre.
Stirling&GlengoyneDistillery[Saturday17thApril] Advancedregistrationwasrequiredforthistrip.
FromGlasgowwedriveto themedievalcityofStirlingtovisitStirlingCastle,whichoverlookstheancientcityofStirlingandisoneofthehistoricbuildingsthathavecometosymbolisethespiritofScotland. WecontinuetoTheTrossachsalongtheshoreofLochVenacharthenclimbthedramaticDukesPasstotheprettyvillageofAberfoyle. TheQueenofScotland’slakes-LochLomond-issuretoputasonginyourheart! LochLomondisthelargeststretchofinlandwaterinBritain. We'llmakeastopatLochLomondShoreswhereyoucanenjoy thespectacularscenerybeforeourlaststopofthedayistoprettyGlengoyneMaltWhiskyDistillerywhere, aswellashavingabehindthescenestourtolearnallaboutthedistillersart, therewillbeachancetotastethefinishedproduct!
Eatingoutinthewestend
TheList isanindependentlimitedcompanybasedinScotlandfounded, inOc-tober1985topromotethewiderangeofarts, eventsandentertainmenttakingplaceeachyearinScotland. Thecompanymaintainstheawardwinningweb-site www.list.co.uk, wheredetailedandwide-rangingreviewsoftheeatinganddrinkingsectorinScotlandcanbefound. Belowwehavereproduced(withkindpermission)extractsfromtheList'sguidetoeatingoutinGlasgow'sWestEnd.Seealso http://www.list.co.uk/places/restaurants/where:g12/
9
Key: B -Budget; S -StudentFriendly; V -vegetarianoptionsaccountfor1/4ofmenu; W -wi-fi; L -latedining. H -HitList
AshokaAshtonLane (L,V) 19AshtonLaneGlasgow, G128SJ,Foodserved: Mon–Thunoon–midnight; Fri/Satnoon–1am; Sun5pm–midnight. Capacity: 68.TheAshtonLanebranchisperhapsAshoka’smostdesirableoutlet, situatedintheheartoftheWestEnd’squaint, cobbledeatinganddrinkingstripanddecoratedinshadesofcoolorangeandbrownwithalargecolourfulmuralofanIndianstreetscenecoveringonewall. Thefoodisyourtypicalmixofclassiccurries, dosasandtandooris(there’snotahugeamountofdifferencemenu-wiserestauranttorestaurantacrossthechain). It’sallwellcooked, inexpensiveandplentifulstuff,withafewScottishtwistssuchashaggispakora.
TheBigBlue (B,S,V) 445GreatWesternRoad, Glasgow, G128HH,Foodserved: Mon–Thu&Sunnoon–10pm; Fri/Satnoon–10.30pm. Capacity: 56.A spaciouspatiowithrelaxingviewsovertheriverKelvin, Mediterranean-styleinteriorswithtwistedirondécor, bleachedwallsandastylishbar, BigBluere-mainsafunkyhang-outforcitydwellersofallages. ThemenucoverseverybasefromburgerstosteaktopastatoTexMextopizza.
Brel (S) 9–43Ashton Lane, GlasgowG128SG,Foodserved: Mon–Sunnoon–10pm.Capacity: 60.BelgianbarandrestaurantBrelhasbeenafixtureontheWestEnd‚squaintAshtonLane forover12years. Downstairs, thewhite tiledwallsandheavywoodendoors(whichareopenedonwarmdays), givethemainrestaurant–aconvertedstable–arusticfeel. Upstairs, theatmosphericwinebarSergeisanappealingspotforanafterdarkquaffandlightbitebyflickeringcandlelight.
Budda (B,S,V) 8CresswellLane, Glasgow, G128AA,Foodserved: Mon–Satnoon–10pm;Sun12.30–10pm. Capacity: 250.Lodgedon the cobbles of theWest End’sCresswell Lane, BarBuddahas es-tablisheditselfasasports-bar-come-restaurantand, morerecently, alate-nightfoodhaunt. Servinguphigh-qualitypubfooduntil2amattheweekends, Buddaboastsamenuofmostlyburgers, pizzasandsandwiches.
CaféAndaluz (B, L,V) 2CresswellLane, Glasgow, G128AA,Mon–Satnoon–11pm;Sun12.30–10.30pm. Capacity: 130.CaféAndaluz resonateswith aNorthAfrican feel viaMoorish decor. Goodseafood.
CaféAntipasti (B,V) 337ByresRoad, Glasgow, G128UQ,Sun–Thu9am–11pm; Fri/Sat9am–midnight. Capacity: 50.Between the fairy lightsand rusticpine tablesandfittings, youmightbe sur-prisedonfirstimpressionstolearnthatCaféAntipastionByresRoadisanItalianrestaurant. Good, unpretentiousfood.
Chow (B,L) 98ByresRoad, Glasgow, G128TB,Foodserved: Mon–Thunoon–2.15pm,5–11.30pm; Fri/Satnoon–2.15pm, 5pm–midnight; Sun4.30–11.30pm. Capacity: 45.ChowdoesnotfeellikeyouraverageChineserestaurant. Itsmanyregularsprizethefriendlyneighbourhoodvibeandpared-downmoderndécor-andthefood’sfarfromaveragetoo. Canfeelcrowded, though.
DiMaggio’s (B,L) 61RuthvenLane, Glasgow, G129BG,Foodserved: Sun–Thunoon–10.30pm;Fri/Satnoon–11.30pm. Capacity: 125.
Kember&Jones (B,V) 134ByresRoad, Glasgow, G128TD,Mon–Fri8am–9pm; Sat9am–9pm; Sun9am–5pm. Capacity: 36.Kember&JonescallsitselfaFineFoodEmporiumwithoutexaggeration–thisroomycaféandcontinentaldeli reallydoes stock someof the freshest, high-qualitybreakfast, lunch, dinnerandsnackeatsyou’llfindinGlasgow.
Koh-i-Noor (L) 12GibsonStreet, Glasgow, G128NX., Foodserved: Sun–Wednoon–1am;Thu–Satnoon–3am.
10
There’salarge, classicIndianmenu, withburgersandkebabstoo. Onceordersareplacedit’snicetobeabletopeerbeyondthecounterandseeamealbeingpreparedwithskillandcare. Punjabimasalaistypical: aclean, creamyheatfromthesauce, ahintofcumin.
TheLeftBank (B,S,V) 33–35GibsonStreet, Glasgow, G128NU,Foodserved: Mon–Fri9am–10pm; Sat/Sun10am–10pm. Capacity: 60.TheLeftBankboastsalltheunderstatedcoolofabarkitchenwhileatthesametimeremainingasrelaxedandversatileasacafébar. ExtensiveVeganoptions.
Mezzo@TheLoft (S) TheGrosvenorTheatre,AshtonLane, Glasgow, G128SJ ,Foodserved: Mon–Satnoon–10pm; Sun11am–10pm. Capacity: 120.A barn-likespaceabovetheGrosvenorCinema, theupstairsrestauranthasnowbeenrevampedwitharusticItaliantheme, withanambitiousmenuemphasisingpeasantdishes, cookedfamily-style(andtheyencouragethemtobesharedthatwaytoo).
NakedSoup (B) 6KerslandStreet, Glasgow, G126BL,Foodserved: Mon–Fri8.30am–8pm;Sat10am–6pm; Sun11am–6pm. Capacity: 20.AlthoughNakedSouphasawiderangeoffoodoptionsonitsmenuincludingasandwiches, saladsandbreakfast, theclueisinthename: thisplacedoesexactlywhatitsaysonthetin.
ÒranMór (B, S) 731–735 GreatWestern Road, Glasgow, G12 8QX, Food served:Mon–Sat9am–9pm; Sun12.30–9pm. Capacity: 140.ThegrandlookingÒranMór, aconvertedsandstonechurchoverlookingByresRoadandtheBotanicGardens, attemptstocaterforthevariedwantsoftrendyWestEndlocalsbybeingallthingstoallpunters: restaurant, club, theatre&bar.Offersgluten-freeoptionsandwheelchairaccess.
Paperino’sWestEnd (L) 227ByresRoad, Glasgow, G128UD., Foodserved: Mon–Sunnoon–10.45pm. Capacity: 180.Paperino’sthreebranchesinGlasgow, allservingtraditionalItaliancuisine, be-ganin1991withtherestaurantonSauchiehallStreet. Thewhite-washedwallsandterracottatilesonthefloorisadecorativethemethattheownersrepeatedwhentheyopenedtheByresRoadbranchin2005. Bigger, brighterandshinier,thenewerrestauranthasacontemporaryatmosphere. A goodselectionofap-petisersincludesbruschettas, antipastoandplentyofvegetarianoptions, suchasstuffedmushroomsandmozzarellasticks.
LaParmigiana (H,V) 447GreatWestern Road, Glasgow, G128HH., Food served:Mon–Satnoon–2.30pm, 5.30–10.30pm. ClosedSun. Capacity: 50.LaParmigianaisaproper, old-schoolItaliandiningexperience, withgracious,knowledgeable–ifslightlysolemn–Italianwaitersinlongstarchedaprons, amenuthatshowcasesaccomplishedItaliancooking, andawinelistthatwouldnotlookoutofplaceinarespectedrestaurantinRome. Andafter30yearsontheGlasgowsceneithasjustregaineditstwoAA rosettes. Deep, richredwalls, crisplinen, angledwoodentablesandhushedtonesallconspiretocreateaserious,grown-upfoodieexperience.
StravaiginCaféBar (B,V) 28GibsonStreet, Glasgow, G128NX,Foodserved: Mon–Fri10am–10.30pm; Sat/Sun11am–10.30pm. Capacity: 85.A WestEndinstitution, StravaiginCaféBaroffersallthefashionableandlocallysourcedeatingofthemainrestaurantdownstairsinthebasement, butinamorerelaxedsetting, andaspopularwithfamiliesasitislocalpopstars. Gluten-freeoptionsandwheelchairaccessavailable; outdoortablesforsmokers.
Ubiquitous Chip (H) 12 Ashton Lane, Glasgow, G12 8SJ., Food served: Mon–Satnoon–2.30pm, 5.30–11pm; Sun12.30–3pm, 6.30–11pm. Capacity: 130.Therestaurantconsistsofaglass-roofed, cobbledcourtyard liberally suppliedwithleafyplantsandasmallfishpond, givingitapleasantoutdoor/indoorfeel.Theserviceisslick, professionalandwarm. Theever-changingmenuisexcit-ingtoreadletalonesample, withtheemphasisoninventivedishesusingfreshingredients. Theimpressivewinelistwillleaveyoustrugglingtochoose.
11
LaVallée Blanche (H) 360Byres Road, Glasgow, G12 8AY., Food served: Tue–Frinoon–2.15pm, 5.30–10.30pm; Satnoon–11.30pm; Sunnoon–10.30pm. ClosedMon.Capacity: 76.LaValléeBlanchesucceedsinshowingsensitivitytoshrinkingbudgetswithoutcompromisingontaste. Justasitsnameandcosychaletinspireddécorimply,the‘WhiteValley’turnsoutthesortoftraditionalFrenchfoodyoucoulddevourafteradayinthemountains. Themenuchangesthroughouttheyeartofavourseasonallocalproduce.
TheWeeCurryShop (B) 23AshtonLane, Glasgow, G128SJ,Foodserved: Mon–Thunoon–2.30pm, 5.30–10.30pm; Fri/Satnoon–11pm; Sun5.30–10.30pm. Capacity: 31.Ifchainrestaurantsare theanathematogoodeating, thenitsgoodtosee theMotherIndiastablecontinuingtodefyreceivedwisdomwiththeirgrowinglineofWeeCurryShops. TherearebranchesalsoinByresRoadandatCowcaddens.
Usefulnumbers, andemergencyinformation
GlasgowTaxis(hackneycabs)01414297070. LocalTaxiRanks: Hillheadsub-waystationandoppositeBotanicalGardens (GreatWesternRoad/ByresRoadintersection).
PrivateHire: WestEndRadioCars01419547070, CanniesburnTaxis01419563333, GlasgowAirportTaxis01418886363.
PublicTransport TravelineScotland http://www.travelinescotland.com/welcome.do, 08712002233(chargesvary).
StrathclydePartnershipforTransport(SPT) http://www.spt.co.uk/
FirstbusGlasgow http://www.firstgroup.com/ukbus/scotland/swscot/home/
Scotrail http://www.scotrail.co.uk/, 08457484950(NationalRailEnquiries).
GlasgowUniversity contacts(fromaninternalphone, diallast4digits)switch-board01413302000, NAM2010RegistrationArea01413300157, MediaRe-lationsOfficer(StuartForsyth)01413304831.
RAS PressOfficers RobertMassey07941248035, AnitaHeward07756034243
Healthandemergencyservices
TheemergencyphonenumberintheUK is999.
AccidentandEmergencyWesternInfirmaryDumbartonRoadGlasgow, G116NTPhone: 01412112000
EmergencydentaltreatmentGlasgowDentalHospitalandSchool(Call01412326323–nowalk-in)378SauchiehallStreetGlasgow, G23JZEveningserviceviaNHS24on08454242424http://www.nhs24.com.
Doctor'ssurgeries26BankStreetGlasgow, G128NDPhone: 01413395513
31BuckinghamTerraceGlasgow, G128EDPhone: 01412116210
Pharmacies277ByresRoadGlasgow, G128TLPhone: 0141339195408:00–20:00
1278ArgyleStreetGlasgow, G38AAPhone: 0141339335308:30–18:00
693GreatWesternRoadGlasgow, G128RAPhone: 0141339001209:00–21:00
12
Security
GlasgowWestEndPoliceOffice(Open24hours)609-611DumbartonRoadGlasgow, G116HYPhone: 01415323592
GlasgowUniversityCampusSecurityGatehouseUniversityAvenue01413304444orx4444fromanyUniversityphone
13
Ses
sion
s Monday12th, 1545–1730Bute P01: GalaxyFormationandEvolutionintheLow-RedshiftUniverse
WithMulti-WavelengthSpectroscopicSurveysG255 P02: MassiveStars: NewViewsoftheirFormationandProgenyG226 P03: 10YearsofCluster: thePast, PresentandFutureofMulti-point
MeasurementsofSpacePlasmasFore P04: NewViewsofSolarActiveRegionsfromHinodeandSTEREO
G466 P05: STFC CurrentFacilities
Tuesday13th, 1045–1230G255 P06: ScienceontheWaytoSKA -Session1Bute P07: FirstresultsfromtheHerschelSpaceObservatoryG226 P08: MagnetosphericphysicsofJovian-typeplanetsandUltra-cool
dwarfsFore P09: UKSP /MIST MissionsForum: theStateoftheArtandFuture:
OpportunitiesG466 P10: SoftwareAstronomy: HowtoDoAstronomybyLookingThrough
aComputer
Tuesday13th, 1545–1730Bute P11: TheDarkArtofDarkMatter-Session1G466 P12: WaterintheSolarSystemandBeyondG226 P13: MagnetospheresandIonospheresThroughouttheUniverseFore P14: MagneticCouplingoftheSolarAtmosphere:
Magneto-SeismologyoftheSolarAtmosphereG255 P15: VISTA:PerformanceandSurveys
Wednesday14th, 1045–1230Bute P16: ScienceontheWaytoSKA -Session2G466 P17: A NewErainAstrochemicalStarFormationG226 P18: GeneralMIST ScienceSession1Fore P19: EnergeticParticlesintheSolarSystemandAstrophysical
Plasmas: ObservationsandTheoryG255 P20: ExplosionsintheDistantUniverse-Session1
Wednesday14th, 1545–1730Bute P21: TheDarkArtofDarkMatter-Session2G466 P22: DisksandStarsatExtremelyHighAngularResolutionFore P23: MagneticReconnection
G226 P24: SolarInfluencesintheHeliosphereG255 P25: ExplosionsintheDistantUniverse-Session2
Thursday15th, 1045–1230Bute P26: TheSloanDigitalSkySurvey: theLegacyandFutureG466 P27: StellarPopulationsinGalaxiesG226 P28: GeneralMIST ScienceSession2Fore P29: ModellingofDynamicSolarPlasmas
G255 P30: PulsarAstrophysics
Friday16th, 1045–1230Bute P31: TheRoleofFeedbackinGalaxyEvolutionG226 P32: StellarandExoplanetaryMagnetismG466 P33: PublicEngagementinAstronomy, SolarandSolarSystemPhysicsFore P34: UKSP GeneralSession
G255 P35: NewTechnologiesforFutureInstruments, TelescopesandMissions
P01 GalaxyFormationandEvolutionintheLow-RedshiftUniverseWithMulti-WavelengthSpectroscopicSurveys[2010April12, 15:45, p43]
WecannowstudythelowredshiftUniverse(z<0.5)usingextensivepopulationstatisticswithverylargegalaxynumbersandhighredshiftcompletenesslevels.Inthissession, welookforwardtocontributionsonnewgalaxysurveyanalyses,whichmakeextensiveuseofmulti-wavelengthdatasetsbycombininginforma-tion fromSDSS,GALEX,Herschel, UKIDSS,etc., onhighlights from thenewGAMA survey, andonresultsfromthemostrecentgalaxyformationmodels.
The"GalaxyAndMassAssembly"(GAMA) surveyisamajorredshiftsurveyforgalaxyformationwithanalreadyuniquespectralenergydistributioncoverage:GALEX-UV,SDSS-optical, UKIRT-NIR,Herschel-FIR andGMRT-radio. GAMAhasmeasuredsince2008over90knewspectraover 150sq.deg., probinginasystematicandcomprehensivemannerthefaintgalaxypopulationoveratimes-panoffourbillionyears(z<0.5).
A NAM sessionfocussedaroundGAMA scienceandsimilarmulti-wavelengthopportunitiesinthelowredshiftUniverseisideallytimedwiththefirstGAMAdatareleaseplannedformid-2010. ThemajorsciencegoalscoveredbyGAMAcomprisemulti-wavelengthgalaxygroupstudies, theevolutionofthebaryoniccontentoftheUniverseandtheefficiencywithwhichgalaxiesformasfunctionofenvironment.
Organisedby: PederNorberg(IfA,UniversityofEdinburgh), IvanBaldry(Liver-poolJohnMooresUniversity)15:45 AaronRobotham: GalaxyAndMassAssembly(GAMA):Thenextgen-
erationsurveyofsurveys.16:05 DavidHill: GAMA photometryandtheCosmicSpectralEnergyDistri-
bution16:20 AlfredoCarpineti: Thecolours, AGN properties, environmentsandstar
formationhistoriesofbulgedominatedpost-mergersinthelocaluni-verse
16:40 CristinaC.Popescu: Modelling theUV/optical FIR/submmemissionfromSpiralGalaxies
17:00 ClaireBurke: ScaleSizeEvolutionofBrightestGalaxies17:15 PosteradvertsPosters LeonidasChristodoulou: GalaxyClusteringUsing Photometric Red-
shiftsEmmaCurtisLake: StudyinggalaxyevolutionwithFMOS (FibreMulti-ObjectSpectrograph)IgnacioFerreras: A newapproachtodisentanglingstarformationhis-toriesfromsurveydataJenniferGupta: A new sampleof "blazars" to study the relationshipbetweenradio-loudAGN andgalaxyformationEdoIbar: Theradiospectralindexofsub-millimetregalaxies.RussellJohnston: RobustmethodstoprobesourceevolutioningalaxyredshiftsurveysLeeKelvin: GAMA:SingleandMulti-ComponentGalaxyModellingErinMacdonald: TheALFALFA HI AbsorptionSurveyMatthewPrescott: RedandBlueSatelliteGalaxiesintheGalaxyandMassAssemblySurveyAwatRahimi: AbundancegradientsinsimulatedgalaxydiscsDmitrijSemionov: ModellingradiationfieldsingalaxiesusinganewradiationtransfercodeBoonKokTan: NGC 2976&NGC 3351: 12CO(3-2)ObservationsanditsCorrelationwithPAH 8um
15
P02 MassiveStars: NewViewsoftheirFormationandProgeny[2010April12, 15:45, p45]
Massivestars, despitetheirrarity, playadisproportionateroleingalaxiessincetheydominatetheirionizingbudget, chemicalenrichmentandfeedback. Thissessionwillfocusupontopicalquestionsrelatingtothepropertiesandevolutionofhighmassstars(mass-loss; significanceofLuminousBlueVariablestage; bi-narystatistics)andtheirprogeny(core-collapseSN;magnetars; GRBs)andwouldinvolve latest results fromTarantula surveyESO largeprogramme, PanSTARRsetc.
Theadventofnewinstruments(SCUBA-2), satellites(Herschel)andprogressinfindingtheearlieststagesofmassivestarformation(egtheIR darkclouds)-aswellastherecentrenewedinterestinmodelsofhowmassivestarsform-alsomakeittimelytoholdasessiondedicatedtotheformationofmassivestars. InthissessionweaimtodrawtogetheralltheexcitingworkbeingdoneintheUK inthisfield, whichwealsohopewillactasacatalysttodrivefuturecollaborationsintheUK communityforALMA projects.
Organisedby: PaulCrowther(UniversityofSheffield), StuartLumsden(Univer-sityofLeeds)15:45 AdamAvison: ProbingSitesofMassiveStarFormation: TheMethanol
MultiBeamSurvey16:05 Heather Cooper: The RMS Survey: Near Infra-Red Spectroscopy of
MassiveYoungStellarObjectsInTheNorthernHemisphere16:25 BenDavies: A MassiveStarisBorn: thecircumstellardisk, envelope,
andbi-polaroutflowofW33A16:40 ChristopherEvans: TheVLT-FLAMES TarantulaSurvey17:00 MatthewAustin: Anultravioletstudyofthetheweakwindproblemin
O stars17:15 AndrewMason: High-MassX-rayBinariesintheNIR:Orbitalsolutions
oftwohighlyobscuredsystems.Posters JaneBuckle: A wide-field, high-resolutionviewofNGC2264
SimonClark: MultiplegenerationsofmassivestarformationinclustercomplexesStaceyHabergham: Type Ibc supernovae indisturbedgalaxies: evi-denceforatop-heavyIMFMarkRushton: TheevolutionofthepeculiarvariableV838Monocero-tis2002-2009
P03 10YearsofCluster: thePast, PresentandFutureofMulti-pointMeasurementsofSpacePlasmas [2010April12, 15:45, p46]
In2010, ESA'sClustermissionwillhavebeenorbitingtheEarthfor10yearsmak-ingmeasurementsofthemagnetosphere, bowshockandsolarwind. Duringthistime, Clusterhashelpedtoimproveourunderstandingofvariousaspectsofso-larterrestrialandplasmaphysicsincludingmagnetosphere-ionospherecoupling,wavesandcurrentsinthemagnetosphere, reconnectionandfluxtransport, andplasmashocks. Inthecomingyears, Clusterwillbeabletomakethefirstmulti-pointinvestigationsofauroralaccelerationprocesses. Withproposalsfornewmulti-spacecraftmissionsunderconsideration, andwithClusterhavingreachedthismilestone, itistimelytoreviewthese10yearsworthofobservationsandcon-siderhowtheseobservationscanhelpusinpreparingforfuturemulti-spacecraftmissionssuchasCross-ScaleandMMS.
Organisedby: ColinForsyth(UniversityCollege, London, MSSL),AndrewWalsh(UniversityCollege, London, MSSL),AndrewFazakerley(UniversityCollege, Lon-don, MSSL),ElizabethLucek(ImperialCollege, London), MattTaylor(EuropeanSpaceAgency)
16
15:45 C.PhilippeEscoubet: 10Years of Cluster: HighlightsofMulti-pointMeasurementsinSpacePlasmas
16:15 KhuromKiyani: UsingCluster’sobservationsofthesolarwindtoinves-tigatecollisionlessplasmaturbulence--currentresultsandoutlookforthefuture
16:30 AndrewWalsh: TheMagnetotailPlasmaSheetRevisited: ClusterPEACEStatistics
16:45 JonathanEastwood: Averagepropertiesofthemagneticreconnectioniondiffusion region in theEarth’smagnetotail: 2001–2005Clusterobservationsandcomparisonwithsimulations
17:00 RogerDuthie: DoBBF eventscontributetoinnermagnetospheredipo-larisation? A threeyearstatisticalstudyusingconcurrentClusterandDoubleStarobservation
17:15 ColinForsyth: Multi-spacecraftobservationsofauroralelectronaccel-erationbyCluster
Posters MikeHapgood: ExtendingCluster JSOC scienceoperationsover thepasttenyears
MattTaylor: Here, thereandeverywhere: gettingafeelforboundarylayerevolutionusingmultipointmeasurements
P04 NewViewsofSolarActiveRegionsfromHinodeandSTEREO [2010April12, 15:45, p48]
Sincetheirlaunchin2006, theHinodeandSTEREO spacecraftshaveprovideduswithnewinsightsintothephysicsofsolaractiveregions. ThecombinationofthreetelescopesaboardHinodeisofferingunprecedentedcoveragefromopticaltoX-raystherebyenablingstudiesofthecouplingbetweendifferentlayersofthesolaratmosphere. Using theobservationsrecordedby theExtreme-ultravioletImagingSpectrometer(EIS) aboardHinodewehavemeasuredphysicalplasmaparameterssuchaselectrondensity, temperatureandflowsinactiveregionsasawhole, aswellas in individualcoronalstructures. TheEUV ImageraboardSTEREO has provideduswith true 3-dimensional topologyof active regions.ThenewobservationalresultsobtainedbyHinodeandSTEREO haveprovideduswithsomeveryimportantconstraintsonthetheoreticalmodellingofactiveregionloops. Inordertoexplainthenewobservationstherehavebeensignificantadvancesinthemodellingofactiveregionloops. Therefore, itisworthwhileandtimelythatwecompareourtheoreticalmodelswithobservationalresults.
Organisedby: AlisonWallace(UniversityCollege, London, MSSL),HelenMason(DAMTP,Cambridge), GiuliodelZanna(DAMTP,Cambridge)
15:45 AlanHood: Whatcantheorydoforyou?
16:00 GiulioDelZanna: Hinode/EIS observationsofactiveregionloops
16:15 LenCulhane: PlasmaMotionsandMagneticReconnectionHeatinginthe2007, May19Flare
16:30 DurgeshTripathi: Activeregionmoss: basicphysicalplasmaparame-tersandtheirtimevariability
16:45 SarahMatthews: Coronalsignaturesofasunspotlight-bridge
17:00 LucieGreen: WhatcanHinodeobservations tellusabouteruptionsfromsigmoidalactiveregions?
17:15 Posteradverts
Posters CarolineAlexander: X-rayBright PointTopology StudywithHinodeandSTEREO
DavidGraham: ObservationsofflareribbondensitiesusingHinode/EIS
IainHannah: Regularized inversion techniques for recoveringDEMsfromHinode/XRT data
17
RobertO'Neil: Relationshipbetweenmagneticfieldandcoronalout-flowsinactiveregions
SantiagoVargasDominguez: Convectiveplasmaaroundsolarpores
P05 STFC CurrentFacilities [2010April12, 15:45, p49]
ThissessionwillprovideacommunityforumtodiscussthecurrentstatusofUKastronomicalfacilities, includingVLT,Gemini, HerschelandSCUBA2. Thefocuswillbeonscienceresultsandfutureprospects, andcurrentandfuturedevelop-mentsininstrumentation.
Organisedby: DerekWard-Thompson(CardiffUniversity)
15:45 RaySharples: UpdateontheKMOS SpectrographforESO VLT
16:00 DimitraRigopoulou: HerschelandSPICA:pushingthefrontiersintothecoolcosmos
16:15 SimonGarrington: e-MERLIN
16:30 JohnRicher: ALMA:statusreportandfirstscience
16:45 GaryDavis: JCMT andUKIRT:GoodNewsandBadNews
17:00 DavidNutter: EarlyresultsfromSCUBA2
17:15 DavidClements: WhitherUK-LedGround-BasedSubmmAstronomy?
Posters RobertBarnsley: FRODOSpec: RoboticSpectroscopyusingtheLiver-poolTelescope
JoaoBento: A studyoftheSuperWASP detectormaps
NeilMawson: TheLiverpoolTelescope: ObservationswiththeSTILT(SmallTelescopesInstalledatLT) widefieldinstruments
P06 ScienceontheWaytoSKA -Session1 [2010April13,10:45, p50]
BothEuropeanandUK visiondocumentsplaceSKA alongsideE-ELT asthekeyground-basedfacilitiesforfutureastronomy. Newradiotelescopesonthepath-waytotheSKA arenowstartingtocomeonlinewithfirstscienceresultsimmi-nentfromeMERLIN,eVLA andLOFAR.Intheseparallelsessionswewillshow-casetheseresultsalongsidethosefrommorematureinstrumentsliketheGMRT(e.g jointGMRT/Herschel surveys). Plans for involvement of theUK sciencecommunityinSKA anditsprecursors(ASKAP andMeerKAT) willbeoutlined.
Organisedby: MattJarvis(UniversityofHertfordshire)
10:45 SteveRawlings: PathwaytotheSKA
11:10 JohnMcKean: EarlyresultsfromthecommissioningofLOFAR
11:25 AlanPenny: A SETI pilotprogrammewithLOFAR
11:40 MattJarvis: TheMeerKAT DeepContinuumSurvey
12:00 PrinaPatel: RadioWeakGravitationalLensingwithVLA andMERLIN
P07 FirstresultsfromtheHerschelSpaceObservatory [2010April13, 10:45, p50]
HerschelwaslaunchedinMay2009andstartedtakingsciencedatainOctober2009. ThefirstscientificresultsfromthismissionwillbeavailableintimeforNAM,allowingtheUK astronomicalcommunityafirstlookatsciencefromthismajorUK andEuropeanmission. Thetimelinessofthissessionislikelytoleadtopressandpublicinterest.
Organisedby: DaveClements(ImperialCollege, London)
10:45 MattGriffin: Herschel: statusandin-orbitperformance
18
11:00 AnthonySmith: InitialresultsfromHerMES:theHerschelMulti-tieredExtragalacticSurvey
11:15 EmmaRigby: TheHerschel-ATLAS:A firstlook
11:30 MatthewSmith: TheHerschelVirgoClusterSurvey(HeViCS)
11:45 DerekWard-Thompson: EarlyHerschelResultsonStarFormation
12:00 NeilPhillips: FirstresultsfromtheDEBRIS survey
12:15 RogerWesson: SPIRE FTS spectraofthreecarbon-richevolvedobjects
Posters HarsitPatel: SWIRE 70micronselectedGalaxies: FollowupandLumi-nosityFunction
P08 MagnetosphericphysicsofJovian-typeplanetsandUltra-cooldwarfs [2010April13, 10:45, p51]
Currentevidencesuggests thatultracooldwarfsbridgethegapbetweensolar-typestarsthatexhibitcoronalactivityandjovian-typeplanetspossessinglarge-scalemagnetospheresandneutralatmospheres. Evidenceforthisplanet-likebe-haviorhasbeenobservedintheradioregime, whereultracooldwarfshavebeenfoundtoproduceperiodicpulsesofextremelybright100%circularlypolarizedradioemission. Thegasgiantsofthesolarsystem–particularlyJupiterandSaturn–havebeenthesubjectofmuchintensiveresearchwithinthelastdecade. SpacemissionssuchasGalileoandCassinihavegivenusunprecedentedinsightintothephysicalprocesseswhichshapethemagneticfields, plasmapopulationsandauroraeoftheseplanets. It is thusanexcellentopportunityforNAM tobringtogethertheultracoolstarcommunityandtheplanetarycommunityandtohigh-lighttheexcellentresearchbeingdoneinmagnetosphericphysicsbeyondtheEarth.
Organisedby: GerryDoyle(ArmaghObservatory), NickAchilleos(UniversityCollegeLondon)
10:45 ChrisArridge: Giantplanetmagnetospheres: JupiterandSaturn
11:10 GreggHallinan: Dynamicspectraofindividualradiopulsesinanul-tracooldwarf
11:30 DavidSouthwood: Sourceofperiodicradioemission; lessonsfromSat-urn
11:45 AlexeyKuznetsov: Numericalsimulationoftheelectron-cyclotronmaserinstabilityinthemagnetospheresofbrowndwarfs
11:55 JonathanNichols: VariationofSaturn'sUV aurorawithSKR phase
12:10 StuartLittlefair: UltraspecObservationsofTVLM 513-46546
12:20 PaulineLang: ThePeculiarbehaviourofRadioEmissioninFullyCon-vectiveStars
Posters RobertKing: PhysicalParametersofUltracoolDwarfs: TheYoungandTheOld
AdamMasters: Structure anddynamics of the boundary of Saturn'smagnetosphere
JaphethYates: Influenceofupstreamsolarwindconditionsonatmo-sphericflowsatJupiter
ShenghuaYu: Mapping radioemitting-regionon low-mass starsandbrowndwarfs
P09 UKSP /MIST MissionsForum: theStateoftheArtandFuture: Opportunities [2010April13, 10:45, p52]
Thissessionwillbesplitintotwoparts: TheStateoftheArtwillreviewthecurrentstatusofUK involvementinupcomingmissions; FutureOpportunitieswillbeanopencommunitydiscussiononfuturemissionsandopportunitiesbeyondand
19
outsidethecurrentCosmicVisionsprogramme. Thestatusofcurrentmissionsandfacilitieswillbepresentedinanaccompanyingpostersession. Thisisyourchancetovoiceyouropiniononwherewemovenextinscienceatacrucialtime!"
Organisedby: DavidWilliams(UniversityCollege, London, MSSL),ColinForsyth(UniversityCollege, London, MSSL),LouiseHarra(UniversityCollege, London,MSSL)
10:45 RobertWalsh: NASA SDO,itsscienceandtheUCLandata-hub
11:00 RichardMarsden: SolarOrbiter: exploring theSunandHeliosphereconnection
11:15 MicheleDougherty: EuropaJupiterSystemMission
11:30 MikeHapgood: Scienceopportunitiesforgeospacestudies?
Posters DanielleBewsher: Determinationofthephotometriccalibrationandlarge-scaleflatfieldoftheSTEREO HeliosphericImagers: I.HI-1
ChrisCarr: TheRosettaPlasmaConsortium
AndrzejFludra: SOHO CoronalDiagnosticSpectrometer
RichardHarrison: TheSTEREO Mission
MarkLester: SuperDARN UK:A newresource tostudyof theupperatmosphere
ElizabethLucek: ClusterFGM:currentandfuturescientificopportuni-ties
ChristopherOwen: SolarOrbiter: TheSolarWindAnalyserInvestiga-tion
JianSun: HinodeUnveilsA NewSun
P10 SoftwareAstronomy: HowtoDoAstronomybyLookingThroughaComputer [2010April13, 10:45, p54]
Increasingly, astronomyishappeninginsoftware. Thisisn'tjustthereductionoftelescopedata(theoldStarlink/IRAF world, wherethesoftwarewasjustanaspectofobservationalastronomy), butastronomywherethecomputeristheprimaryinstrumentdeliveringthescience. Thiscoverssimulationsanddatamining, butmostrecentlyalsovarioustypesoffundamentallyonlineapproachestohandingtheever-intensifyingdatadeluge, includingvirtualobservatory, crowdsourcing,socialastronomy, andthesemanticweb.
Inthisspecialsessionwewillbringtogetherleadersinthevariousstrandsofsoft-wareastronomy. TheUK hasaleadingroleinthis(arguably)newsubdiscipline,andthisspecialsessionwillbuildthiscommunity, andcementitslinkstothemore... traditionalroutesfromphotonstoelectrons.
Organisedby: NormanGray(UniversityofGlasgow)
10:45 IntroductoryRemarks
11:00 DuncanForgan: NativeSyntheticImagingofSmoothedParticleHydro-dynamicsSimulations
11:20 AnnaMariaMassone: SoftwaretoolsforprocessingRHESSI visibilities
11:40 ChrisLintott: SupportingDistributedScience: RunningGalaxyZoo
12:00 MarkJones: Developingskillsfor“softwareastronomy”: aninnovativedistancelearningprojectforOpenUniversitystudents
12:20 AvonHuxor: GraphicInterfacestoExplanatoryAnalysisofAstronomi-calImageDatabases
Posters RobBlake: TheWFCAM ScienceArchive
JohnBrooke: DataIntegrationinHeliophysics
OliverButters: TheSuperWASP publicarchive
20
TobiaCarozzi: VOeventstriggeredbygravitywaves
NigelHambly: NewinfraredandopticalimagesservicesintheVO
MarkHolliman: VirtualObservatoryServicesatWFAU
BonnieSteves: ThehierarchicalstabilityofexoplanetarysystemsofBi-narystarsusingtheCaledonianSymmetricFour-Bodymodelwithanewglobalregularisationalgorithmtohandlecloseencounters
P11 TheDarkArtofDarkMatter-Session1 [2010April13,15:45, p56]
Thegoalofthissessionistounderstandthemysteriousdarkmatterthatcom-prises95%ofthemattercontentoftheUniverse. TheUK isattheforefrontofresearchinthefieldsofCosmologyandParticlePhysicswithstrengthsinboththeoryandobservations. Wewelcomeanyresearcherintheoryorobservation,fromallfields, workingtowardsthegoalofunderstandingdarkmatter. Togetherinthissessionwewilldiscusskeyquestionssuchas: “howcanwebetterexploitsynergiesbetweendirectandindirectdetection?”Toaiddiscussion, inadditiontothetwoscheduledparallelsessionstherewillbea20-30personbreak-outsession, tobeheldonthemorningof14thApril. Ouraimistofosteracollabo-rativeenvironmentatthemeetingthatwillleadtostrongUK-ledresearchinthisrapidlydevelopingfield.
Organisedby: CatherineHeymans(IfA,UniversityofEdinburgh), RichardMassey(IfA,UniversityofEdinburgh), TomKitching(IfA,UniversityofEdinburgh)
15:45 PawelMajewski: Directdetectionofdarkmatter
16:10 JustinRead: DarkMatterintheMilkyWay
16:35 JorgePenarrubia: The impactofdarkmattercuspsandcoreson thesatellitegalaxypopulatio
16:50 AlinaKiessling: ApplicationsofaNewandRapidSimulationsMethodforWeakLensingAnalysis
17:00 EdwardThomson: Wave-mechanicsofLargeScaleStructure
17:10 JakobJonsson: WeighinggalaxiesusinggravitationallylensedSNLS su-pernovae
17:25 Posteradverts
Posters ChrisBrook: Dodarkmatterhaloshavecusps?
OlafDavis: Extremevaluestatistics: predicting the frequencyof thedensestclustersandsparsestvoids
MartinFeix: TeVeS andthestraightarcofA2390
IgnacioFerreras: Probingthedarkmatterhalosofearly-typegalaxiesvialensing
HodaGhodsi: SuddenFutureSingularitymodelsasanalternativetoDarkEnergy?
GülayGürkan: Thenewpathtotimedelays?
VictoriaHamilton-Morris: LoCuSS:WeakLensingAnalysisof21GalaxyClustersatz=0.15-0.3
CatherineHeymans: Probing theDarkUniversewithWeakLensingTomographyandtheCFHTLS
DanielJohn: A NewPixonWeakLensingClusterMassReconstructionMethod
CraigLawrie: Theimpactofdelensinggravitationalwavestandardsirensondeterminingcosmologicalparameters
HongshengZhao: BrightIdeasandDarkThoughts: "UniversalBaryonicScale"at"MaximumHaloGravity"
21
P12 WaterintheSolarSystemandBeyond [2010April13,15:45, p57]
Thissessionaimstocutacrosssomeofthetraditionalsubjectareasinastrobiol-ogy, bringingpeopletogethertoconsidertheorigin, distributionandactionofwaterinthegalaxy. TopicscoveredwillspantherangefromwaterintheSolarSystem–i.e. theMoon, Marsandasteroids, andicybodies(e.g. comets, Europa)–toexoplanetaryatmospheres.
Organisedby: MonicaGrady(OpenUniversity)
15:45 PedroLacerda: TheDensitiesofKuiperBeltObjects
16:00 HenryHsieh: TheMain-BeltComets: Long-livedIceintheInnerSolarSystem
16:15 JayFarihi: TheFrequencyandCompositionofWater-RichExtrasolarAsteroids
16:30 IngoWaldmann: Characterisationofexoplanetaryatmospheres
16:45 DavidKipping: NightsidePollutionofExoplanetTransitDepths
17:00 MikakoMatsuura: ObservationsandmodellingofwatervapourlinesintheHerschelSPIRE FTS spectrumoftheluminousred-supergiant, VYCanisMajoris
17:15 AnitaRichards: AmasingWater
P13 MagnetospheresandIonospheresThroughouttheUniverse[2010April13, 15:45, p58]
MagnetospheresareubiquitousthroughouttheUniverse, beingfoundininter-stellargasclouds, intheenvironmentsofblackholesandotherdegenerateob-jectsaswellasaroundplanetsandstars. Galactic, heliospheric, andexoplane-tarymagnetospheresaddyetanotherdimensiontothisimmensevariety. Iono-spheresandionospheric-likecollisionalplasmaenvironmentsarealsoubiqui-tous in planetary environements andmuch of the collisional plasma physicsfoundinplanetaryionospherescanalsobeappliedtoastrophysicalsystemssuchasaccretiondiscs. Thesolarsystemcontainsadiversearrayoffascinatingplan-etarymagnetospheresandionospheres, eachuniquebutsharingthesamefun-damentalphysicalprocesses. Solar systemenvironmentshavebeenexploredusingavarietyof techniquesandsuch investigationshavebenefited fromtheuniqueadvantageofbeingabletoincludein-situmeasurements. Thishasledtoasignificantbodyofunderstandingonspaceplasmaswhichishighlyapplicabletoastrophysicalsystems. Comparativestudiesbetweenplanets(includingEarth)andmoonsthroughoutthesolarsystemallowinvestigationsofawiderangeofphysicalconditions, suchasmagneticfieldconfigurationandcompositionoftheplasma. Comparisonsbetweenplanetaryandastrophysicalenvironmentsrevealinterestingsimilaritiesinsystem-levelbehaviour, suchasphaseshiftsanddriftingperiodsinperiodicplanetaryradioemissionsandtheintermittentbehaviourofsomepulsars.
We invite contributions that discuss the physical processes and structures inastrophysicalandplanetarymagnetospheres, ionospheresandionospheric-likecollisionalastrophysicalplasmaenvironments. Weanticipatepapersthatstudygeneralmagnetosphericandionosphericphysicsleadingtoauniversalunder-standingofmagnetospheresandionospheresandwhichexploretheapplicabilityofcollisionalionosphericplasmaphysicstoastrophysicalplasmaenvironments,suchasaccretiondiscs.
Organisedby: ChrisArridge(UniversityCollege, London, MSSL),BenStappers(UniversityofManchester), AlanWood(AberystwythUniversity), AndyBreen(AberystwythUniversity)
15:45 Introductoryremarks
22
15:50 SteveMiller: TheroleofH3+inplanetaryatmospheres
16:10 PatrickWeltevrede: Radioobservationsofhighlyenergeticpulsars
16:30 ThomasNeukirch: Simplemodelsforclosedfieldlineregionsofthree-dimensionalrigidlyrotatingmagnetospheres
16:45 NicholasAchilleos: TheInfluenceofHotPlasmaPressureonMagne-tosphericStructureatSaturn
17:00 EuanBennet: AlfvénWavesinPartially-IonisedandRecombiningPlas-mas
17:15 RobertKidd: Searching forEvidenceofStarSpots inSTEREO Helio-sphericImagerData
Posters GeraintJones: TheShockingSizeofCometMcNaught
KevinRonald: LaboratoryExperimentstoinvestigatethemechanismsofAuroralKilometricRadiation
AlanWood: IonlosstotheSolarWindfromVenusatSolarMinimum
P14 MagneticCouplingoftheSolarAtmosphere:Magneto-SeismologyoftheSolarAtmosphere [2010April13, 15:45, p60]
Highresolutionobservations(TRACE,HINODE,STEREO) arerevolutionizingourviewsandunderstandingofphysicalprocessesinthesolaratmosphereandtheconnectivitybetweenvarious regionsandphenomena takingplace in theso-laratmosphere. Combiningobservablepropertiesofwavesandoscillationsinvariousmagneticstructureswiththeoretical(includingnumerical)modelling, al-lowusdeterminationof notonlymagnitudeofmagneticfieldsbut also sub-resolutionstructuringusingseismologicaltechniques. Thesessionaimstoreviewrecentadvancesinthefieldofmagneto-seismologyandputindividualdynami-cal/energeticphenomenaintoamuchwiderglobalpicture.
Organisedby: I.Ballai(UniversityofSheffield), R.vonFaySeibenburgen(Uni-versityofSheffield), M.Mathioudakis(Queen'sUniversityBelfast)
15:45 GaryVerth: Magnetoseismologyof thechromospherewith torsionalAlfvénwaves
16:00 DavidJess: ThelinkbetweenSodiumintensityenhancementsandthephotosphericmagneticfield
16:15 TomVanDoorsselaere: Anatomyofaslowwaveinacoronalloop
16:25 SergeiZharkov: Evidenceofmagneto-acousticwavesinphotosphericobservationsofasunspot
16:35 MikeMarsh: ExploitingtheCoronalSlowMode
16:45 RichardMorton: Properties ofMHD waves in plasmawith variablebackground
16:55 DavidPascoe: CoupledAlfvénandKinkOscillationsinCoronalLoops
17:05 PhilipCrockett: BigBrightPoint, SmallBrightPoint, Cardboardbox
17:15 DavidRobertson: Theeffectofdensitystratificationonthetransverseoscillationsoftwoparallelcoronalloops
Posters IstvanBallai: TRACE/EUV observationofdrivenlooposcillations
NickyChorley: Longperiodoscillationsinsunspots
HughHudson: Flaresandglobalwaves, includingseismic
MarialejandraLuna: Longitudinaloscillationsinanexpandinghotcoro-nalloop.
BeniaminOrza: PhasemixingintheSolarCorona
23
P15 VISTA:PerformanceandSurveys [2010April13, 15:45,p61]
VISTA'sfirstScienceruns(10daysofScienceVerification)completedon02-NovandVISTA wasacceptedbyESO inmidNovember. ‘DryRun'surveys(100hrforeachofthesixsurveys)started03-NovandtheVISTA PublicSurveysformallybeginon15-Feb2010.
Whilstitwillbealittleearlytoexpectmuchnewscience, thepurposeofthissessionwillbetoprovideatimelyreportontheperformanceandcapabilitiesoftheas-builtVISTA,andontheprogressandresultssofarfromthefirstdataoftheESO publicsurveyswithVISTA.
Organisedby: JimEmerson(QueenMary, UniversityofLondon)
15:45 JimEmerson: VISTA Performance
15:55 JamesLewis: TheVISTA sciencepipeline
16:05 JamesDunlop: UltraVISTA
16:20 MattJarvis: TheVISTA DeepExtragalacticObservations(VIDEO) Sur-vey
16:35 WillSutherland: VIKING,theVISTA Kilo-degreeInfraredGalaxySurvey
16:50 JosephFindlay: HighredshiftquasarsintheVIKING field.
17:00 RichardMcMahon: TheVISTA HemisphereSurvey
17:15 Maria-RosaCioni: TheVMC survey-I.StrategyandEarlyScienceData
Posters GemmaBagheri: A near-infraredstudyoftheMagellanicSystemwithVISTA.
RossCollins: TheVISTA ScienceArchive
NicholasCross: FindingvariablesusingtheVISTA ScienceArchive
RoaldGuandalini: FirstobservationsofstellarclustersintheLMC fromtheVMC survey
PhilipLucas: VISTA VariablesintheViaLactea(VVV) andnewUKIDSSGPS highamplitudeIR variables
Maria IdaMoretti: Variable Stars in theVISTA near-infraredY, J, KssurveyoftheMagellanicCloudSystem(VMC)
P16 ScienceontheWaytoSKA -Session2 [2010April14,10:45, p62]
BothEuropeanandUK visiondocumentsplaceSKA alongsideE-ELT asthekeyground-basedfacilitiesforfutureastronomy. Newradiotelescopesonthepath-waytotheSKA arenowstartingtocomeonlinewithfirstscienceresultsimmi-nentfromeMERLIN,eVLA andLOFAR.Intheseparallelsessionswewillshow-casetheseresultsalongsidethosefrommorematureinstrumentsliketheGMRT(e.g jointGMRT/Herschel surveys). Plans for involvement of theUK sciencecommunityinSKA anditsprecursors(ASKAP andMeerKAT) willbeoutlined.
Organisedby: MattJarvis(UniversityofHertfordshire)
10:45 TomMuxlow: Thee-MERGE LegacySurvey
11:05 EmmaRigby: Theluminosity-dependenthigh-redshiftcut-offofthera-dioluminosityfunction
11:25 AndyLawrence: OriginoftheCosmicRadioBackground
11:45 HansikKim: Thespatialdistributionofcoldgasinhierarchicalgalaxyformationmodels
12:00 RogerDeane: HighResolutionRadioObservationsofIRAS FSC10214
Posters JoannaBulger: TheOVRO OphiuchusPre-Stellar (OOPS) Survey: A3.4mmContinuumEmissionStudyofCircumstellarMaterial
24
P17 A NewErainAstrochemicalStarFormation [2010April14,10:45, p63]
Thissessionwillprovideanoverviewofcurrentresearchinastrochemistry, bring-ing together thefieldsofobservationalastronomy, theoreticalmodelling, andlaboratoryastrochemistry. TheemphasiswillbeonastrochemicalresearchinareasthatwillreapthebenefitsofcurrentandplannedmissionssuchasJCMT,Herschel, ALMA andJWST,particularlyareasassociatedwithstarformationinboththenearandfaruniverse.
Thisisanexcitingtimeforthestudyofastrochemicalprocessesinthefaruni-verse. Detectionsofwaterice, amorphousandaromatichydrocarbonsatred-shifts 2, anddetectionsintheearlyuniverse(e.g. CO atz 6)areprovidingthestimulus for research into star formation inhigh redshift galaxies, whereverydifferentphysicalparametersareneeded formodels. In thenearbyuniverse,theimprovedspatialandspectralresolutionofferedbynewinstrumentationwillstronglyinfluencemodelsofstarandplanetformation, enabling, evenenforcing,theinclusionofdynamicsinchemicalmodelsof, forexample, nearbycircum-stellardisks. Suchmodelsandobservationsalsorequireinteractionwithdevel-opinglaboratorystudies. Ournewviewofthemolecularcomplexityinthelocalgalaxywillchangedramaticallytheunderstandingofformationprocessesandevolutionarystages.
Organisedby: JaneBuckle(CavendishAstrophysics, Cambridge)
10:45 StevenCharnley: IsotopicFractionationinPrimitiveMaterial: Quanti-fyingtheContributionofInterstellarChemistry.
11:00 EstelleBayet: Extragalactic star formationactivity -propertiesof theverydensegas
11:15 MartinMcCoustra: Photon- and Electron-drivenProcesses inModelInterstellarIces
11:30 GaryFuller: AstrochemistryintheALMA era
11:45 NatalieChristopher: FirstResultsfromSHINING -SurveywithHerscheloftheISM inNearbyINfraredGalaxies
12:00 VictoriaFrankland: TowardsUnderstandingtheFormationofWaterintheInterstellarMedium
12:15 ZainabAwad: Thedeuteriumchemistryinlowandhighmassstarform-ingregions
Posters AliAbdulgalil: LaboratoryStudiesofNon-thermalDesorptionofAce-tonitrilefromIcyGrainMantles
SeanChapman: InvestigatingtheOnsetofSilicateCrystallizationintheEarlyStagesofStarFormation
HelenChristie: ChemistryofdenseclumpsnearmovingHerbig-Haroobjects
KerryHebden: ChemicalevolutioninNGC 6302(theButterflynebula)
NadyaKunawicz: Hotcoremodelsatlowmetallicity
PaulRuffle: TheXgearProject -A NewEra forAstrochemicalMod-elling?
P18 GeneralMIST ScienceSession1 [2010April14, 10:45, p65]
Magnetospheric-Ionospheric-Solar-Terrestrial(MIST) researchconcernsphysicalprocesseswithintheSun-Earthsystem, othersolarsystembodiesandexo-planets;inparticularthesolar/stellarwind, moonsandplanetaryatmospheresandmag-netospheres. TheMIST generalsessionisdesignedtoaddressthoseaspectsof
25
currentMIST researchnotexplicitlycoveredinothersessions, suchasneutralat-mospherescience, ULF wavesandwave-particleinteractions, auroralandiono-sphericelectrodynamics, andground-basedstudiesofthecoupledmagnetosphere-ionosphere system. All researcherswhoare interested inanyaspectofMISTsciencearethereforeinvitedtotakepart.
Organisedby: AdrianGrocott(UniversityofLeicester), EmmaWoodfield(Uni-versityofLancaster), AndrewFazakerley(UniversityCollege, London, MSSL)
10:45 MarkLester: CoordinatedgroundandspaceobservationsofGeospace:A viewfromtheground
11:05 JamesHutchinson: ObservationsofGeomagneticStormsoveraSolarCycle: SomeInitialFindings
11:20 AlanWood: Comparisonsofplasmatransportinthehigh-latitudeiono-spheresoftheEarthandVenus.
11:35 CathrynMitchell: GPS Plasmsphericimaging
11:55 Katie Turnbull: ModellingGeomagnetically InducedCurrents in theNationalGridusingSAMNET.
12:10 MartinFullekrug: SpritesandRelativisticElectronBeamsAboveThun-derclouds
12:25 Posteradverts
Posters EwanDawson: EstimatingtheExtremesinGeomagneticActivityAcrossEurope
TimothySpain: MagneticfieldparallelcurrentsintheUCL-CTIP model
JimWild: Presentdaychallenges inunderstanding thegeomagnetichazardtonationalpowergrids
P19 EnergeticParticlesintheSolarSystemandAstrophysicalPlasmas: ObservationsandTheory [2010April14, 10:45,p68]
Thegenerationofahigh-energynon-thermalparticlepopulationisaprominentfeatureofmanymagneticactivityprocesses insolar systemandastrophysicalplasmas. Examples includeauroralparticleacceleration inplanetarymagne-tospheres, solarand stellarflaresandenergeticprocesses incompactobjectssuchaswhitedwarfs, neutronstarsandblackholes. Thissessionaimstofur-therourunderstandingof thephysicalprocessesunderlying thegenerationofhigh-energynon-thermalparticlepopulations indifferentphysical regimesbygivingresearchersfromdifferentareastheopportunitytopresenttheirworkandexchangetheirideas. Weencouragethesubmissionofpapersonboththetheo-reticalandobservationalaspects, includingtheaccelerationprocess, thepropa-gationandtransportofenergeticparticlesfromthelocationofacceleration, andtheirdetection.
Organisedby: ThomasNeukirch(UniversityofStAndrews), SilviaDalla(Uni-versityofCentralLancashire)
10:45 PhilippaBrowning: ParticleaccelerationattheSun
11:05 AndrewWright: AuroralParticleAccelerationattheEarth
11:25 ChristinaBurge: ParticleAccelerationinthePresenceofWeakTurbu-lenceatanX-TypeNeutralPoint
11:38 MykolaGordovskyy: Particleaccelerationinafragmentingcurrentsheet
11:51 Rim Turkmani: Electrons re-acceleration at the chromospheric foot-pointsofSolarFlares
12:04 HamishReid: SolarFlareAcceleratedElectronTransport through theTurbulentDensityoftheSolarWind
12:17 MichelePiana: Fromelectronmapstoaccelerationmechanismsofen-ergeticparticlesintheflaringSun
26
Posters MarinaBattaglia: ImagingobservationsofX-rayalbedoinacompactdiskflareNicolasBian: ParallelelectricfieldgenerationbyAlfvénwaveturbu-lenceSilviaDalla: RoleoflatitudeofsourceregioninsolarenergeticparticleeventsEwanDickson: MeasurementofAnisotropyinSolarFlareElectronSpec-trausingRHESSI HardX-RaySpectroscopy.KeithGrady: ParticleMotion and EnergyGains in KinematicMHDmodelsofCollapsingMagneticTrapsJingnanGuo: Temporal, Spectral, andSpatialAnalysesofX-rayEmis-sionComponentsinImpulsiveSolarFlaresIainHannah: CantheinfluenceofturbulentdensityperturbationsinthecoronabedetectedinflareX-rayspectrum?ChuanLi: Coronalmagnetic topologyandthesolarsourceofmajorSEP eventsSiming Liu: Stochastic ParticleAcceleration by CompressiveModeswithIncompressiveModeInducedSpatialDiffusionHeatherRatcliffe: Electromagneticemissionfrombeam-generatedLang-muirwavesDavid Speirs: Numerical simulation ofmagnetospheric electron cy-clotronemissionCraigStark: MagnetosphericParallelElectricFields
P20 ExplosionsintheDistantUniverse-Session1 [2010April14, 10:45, p70]
Explosiveextragalactictransientsarenowbeingroutinelydiscoveredacrosstheelectromagneticspectrumcomplementedbydatafromincreasinglysensitivegrav-itationalwaveandneutrinoobservatories. Thecombinationof such facilitiesopensupnewopportunitiesforthestudyoftransientphenomenaincludingGamma-RayBursts, Supernovaeandtidaldisruptionbysuper-massiveblackholes. Weproposeapairof sessionsatNAM2010 todiscusscurrent results in this fast-movingareaandtoencouragecoordinatedresearchcombiningphotonicandnon-photonicdata.
Theproposedsessionshavetwomaingoals: (1)todiscussthemostinterestingrecentdiscoveriesintheexplosiveUniversefromworkingfacilities; and(2)toenhancediscussionandinteractionbetweenthesediversecommunitiesanden-couragenewworkingrelationships. Thesessiontopicswouldbeapproximatelydividedinto:
• Supernovae: newdiscoveriesanddiversityofexplosionphysics;
• GRBs: recenthighlightsandpotentialforthefuture;
• Thepotentialof futuresurveysand facilities forcharacterisingexplosivetransients.
Wewouldparticularlyencourage reports fromthecurrent / futureuseof sur-veysandfacilitiesinvolvingUK partners(e.g. Swift, Fermi, Pan-STARRS,LOFAR,LIGO,MAXI,HESS,CTA).
Organisedby: PaulO'Brien(LeicesterUniversity), StephenSmartt(QueensUni-versityBelfast), JonathanGranot(UniversityofHertfordshire), NialTanvir (Le-icesterUniversity)10:45 MarkSullivan: LuminoustransientsinthedistantuniversewithPTF and
SNLS
27
11:30 MorganFraser: Identifyingandchacterising theprogenitorsof core-collapsesupernovae
11:45 JoanneBibby: SurveyoftypeIb/csupernovaprogenitorsinnearbystar-forminggalaxies.
12:00 ZachCano: TheGRB-SN connection: ExploringGRB progenitorswithmulti-wavelengthobservations
12:15 ValeriuPredoi: Searchforgravitational-waveinspiralsignalsassociatedwithshortGamma-RayBurstsduringLIGO'sfifthandVirgo'sfirstsci-encerun
P21 TheDarkArtofDarkMatter-Session2 [2010April14,15:45, p71]
Thegoalofthissessionistounderstandthemysteriousdarkmatterthatcom-prises95%ofthemattercontentoftheUniverse. TheUK isattheforefrontofresearchinthefieldsofCosmologyandParticlePhysicswithstrengthsinboththeoryandobservations. Wewelcomeanyresearcherintheoryorobservation,fromallfields, workingtowardsthegoalofunderstandingdarkmatter. Togetherinthissessionwewilldiscusskeyquestionssuchas: “howcanwebetterexploitsynergiesbetweendirectandindirectdetection?”Toaiddiscussion, inadditiontothetwoscheduledparallelsessionstherewillbea20-30personbreak-outsession, tobeheldonthemorningof14thApril. Ouraimistofosteracollabo-rativeenvironmentatthemeetingthatwillleadtostrongUK-ledresearchinthisrapidlydevelopingfield.
Organisedby: TomKitching(IfA,UniversityofEdinburgh), RichardMassey(IfA,UniversityofEdinburgh), CatherineHeymans(IfA,UniversityofEdinburgh)15:45 Reviewofthismorning'sbreak-outsession15:55 DavidMiller: UsingtheLHC toprobeDarkMatterinphysicsbeyond
theStandardModel16:20 MarkusHorn: TheZEPLIN-III DarkMatterSearchExperiment16:35 FergusSimpson: UnmodifiedGravity16:50 MatthewWalker: EmpiricalConstraintsontheDarkMatterContentof
DwarfSpheroidalGalaxies17:05 CarlosFrenk: Cosmologyonsmallscales: thestructureof(mostly)dark
matterhalos
P22 DisksandStarsatExtremelyHighAngularResolution[2010April14, 15:45, p72]
ThissessionaimstohighlighttotheUK astronomycommunityrecentresultsandprogressinthefieldofopticalandinfraredlong-baselineinterferometry. Opti-calinterferometrycanpresentlyachieveangularresolutionsashighasverylongbaselineinterferometry(VLBI) andcancombineuptosixtelescopes. Imagingofdisksandstarsatextremelyhighangularresolutioncanbeachievedwiththeexistinginterferometricfacilities. Weinvitecontributionswhichdiscusscurrentresults, encouragecollaborativeresearchandexploitationoftheexistinginstru-ments.
Organisedby: EttorePedretti(UniversityofStAndrews)15:45 ReneOudmaijer: Opticalandnear-infraredinterferometryofstarsand
disks16:10 MyriamBenisty: ThecomplexinnerdisksofHerbigAeBestars16:23 JennyPatience: Investigatingtheinnerdisksofyoungstars16:36 FabienBaron: ImagingwithMIRC attheCHARA interferometer16:49 RachelSmith: Resolvingdebrisdiscsinterrestrialplanetregionswith
MIDI-VLTI
28
17:02 JohnYoung: CharacterisingtheconvectionpatternonBetelgeuse
17:15 Foteini(Claire)Lykou: Dustydiscsaroundevolvedstars
Posters DavidBuscher: ScienceProspectswiththeMagdalenaRidgeObserva-toryInterferometer(MROI)
JamesGordon: ImagingshockfrontsinMiravariables
EttorePedretti: Mappingstar-spotsontheRS CVnbinary ζ And
AlexRea: TheMagdalenaRidgeInterferometerFringeTracker
AnitaRichards: Dosingleoldstarsejectclumps?
P23 MagneticReconnection [2010April14, 15:45, p73]
Magneticreconnectionisafundamentalprocessinastrophysical, solarandmag-netosphericplasmas. Previouslymagneticreconnectionwasunderstoodintermsof two-dimensionalMHD modelswhichsometimes leadtooversimplistican-swersregardingthedynamicsandenergeticsoftheprocess. Nowadaysthree-dimensionalfluidmodels(MHD,Hallormulti-fluid)orkineticmodelsarethestateoftheartandthesemodelsproduceamorecomplexanddiverserangeofreconnectionphenomena. Whilethisnewgenerationofmodelsprovidesmuchmorerealisticanswers, whichcanbebettercomparedwithobservations, theyarealsomorechallengingtounderstand. Weinvitecontributionsfromastrophysics,solarandmagnetosphericphysicsforajointsessionontheoryandobservationsofmagneticreconnection, aprocesswhichiskeytoourunderstandingofplasmadynamics.
Organisedby: GunnarHornig(UniversityofDundee)
15:45 MichaelBareford: A NanoflareDistributionGeneratedbyRepeatedRelaxationsTriggeredbyKinkInstability
16:00 AlisonWallace: Doesmagnetichelicityeffectactiveregionevolutionandenergetics?
16:15 DavidPontin: Regimesofmagneticreconnectionat3D nullpoints
16:30 PeterWyper: 3D MagneticNullpoints: LocalisedFantiltingandTor-sionalReconnection
16:45 Robert Fear: Comparisonofmodels of flux transfer event formationusingpredictedandobservedasymmetry
17:00 AntoniaWilmot-Smith: Relaxationofbraidedcoronalloopsbymultiplesmall-scalereconnectionevents
17:15 ClareParnell: 3-D Magneticreconnectionatseparators
Posters GunnarHornig: Turbulentrelaxationofbraidedmagneticfields
EhsanPedram: A surveyofHXR emissionofseismicallyactiveandquietX-classwhite-lightflares
FionaWilson: PropertiesoftheDistributionFunctionofaVlasov-MaxwellEquilibriumfortheForce-FreeHarrisSheet
P24 SolarInfluencesintheHeliosphere [2010April14, 15:45,p75]
ThissessionwilladdressourcurrentunderstandingoftheinfluenceoftheSunonthesurroundingheliosphericenvironment, andtheopportunitiesforfutureresearchinthisarea. Conventionally, wehaveconductedremotesensingofthenear-Sunenvironmentandhaveperformedinsitumeasurementsfurtheroutintheheliosphere; thishasledtotwodistinctareasoffocus. Howeverinrecentyears, andparticularlywiththeadventoftheSTEREO mission, manynewdataanalysistechniqueshavebeendevelopedthatbridgethisdividebetweenstudiesofthenear-Sunandinterplanetaryspaceenvironments.
29
ThereisstillmuchtolearnaboutthelinksbetweentheSunandtheheliosphere,inparticulartheoriginsoftheambientsolarwindandsolarejecta, theirstructureandevolutionastheypropagateintointerplanetaryspaceandtheirsubsequentinteractionswithplanetsandothersolarsystembodies. Thissessionwilldrawtogetherourcurrentknowledgeofthephysicswithinthesolar-heliosphericen-vironment, whilstaddressingthemethodologiesrequiredtofurtherunderstandandprogressthisareaofscience, withparticularemphasisontheexploitationofmultiplemissions.
AllresearcherswhoareinterestedintheSun-heliosphereconnectionareinvitedtoparticipateandtocontributetothissession.
Organisedby: KimberleySteed(UniversityCollege, London, MSSL),JackieDavies(RutherfordAppletonLaboratory), RichardHarrison(RutherfordAppletonLab-oratory), ChrisDavies(RutherfordAppletonLaboratory)
15:45 Introductoryremarks
15:50 MathewOwens: Probing the evolution of coronal andheliosphericstructureswithsuprathermalelectrons
16:15 AnthonyYeates: Non-potentialenhancementoftheSun'sopenmag-neticflux
16:30 PeterGallagher: PropagationofanEarth-DirectedCoronalMassEjec-tionin3D
16:45 MarekKukula: SolarStormwatch: acrowd-sourcingapproachtoun-derstandingCoronalMassEjections
17:00 SrividyaSubramanian: Small scale transient featuresatcoronalholeboundaries: apossiblesourcefortheslowsolarwind?
17:15 LidiavanDriel-Gesztelyi: Are there imprintsofhotplasmaoutflowsfromactiveregionsinthesolarwind?
Posters RobertBentley: TheHeliophysicsIntegratedObservatory
MarioBisi: A ComprehensiveStudyofthe13-15May2005SolarEvent(s)
ChristopherDavis: AssessingtheaccuracyofCME speedandtrajectoryestimatesfromSTEREO observationsthroughacomparisonofindepen-dentmethods
KimberleySteed: Investigatingtheobservationalsignaturesofmagneticcloudsub-structure
AnthonyWilliams: CharacterisingtheSTEREOHeliosphericImagersig-naturesofCorotatingInteractionRegions
P25 ExplosionsintheDistantUniverse-Session2 [2010April14, 15:45, p76]
Explosiveextragalactictransientsarenowbeingroutinelydiscoveredacrosstheelectromagneticspectrumcomplementedbydatafromincreasinglysensitivegrav-itationalwaveandneutrinoobservatories. Thecombinationof such facilitiesopensupnewopportunitiesforthestudyoftransientphenomenaincludingGamma-RayBursts, Supernovaeandtidaldisruptionbysuper-massiveblackholes. Weproposeapairof sessionsatNAM2010 todiscusscurrent results in this fast-movingareaandtoencouragecoordinatedresearchcombiningphotonicandnon-photonicdata.
Theproposedsessionshavetwomaingoals: (1)todiscussthemostinterestingrecentdiscoveriesintheexplosiveUniversefromworkingfacilities; and(2)toenhancediscussionandinteractionbetweenthesediversecommunitiesanden-couragenewworkingrelationships. Thesessiontopicswouldbeapproximatelydividedinto:
• Supernovae: newdiscoveriesanddiversityofexplosionphysics;
30
• GRBs: recenthighlightsandpotentialforthefuture;
• Thepotentialof futuresurveysand facilities forcharacterisingexplosivetransients.
Wewouldparticularlyencourage reports fromthecurrent / futureuseof sur-veysandfacilitiesinvolvingUK partners(e.g. Swift, Fermi, Pan-STARRS,LOFAR,LIGO,MAXI,HESS,CTA).
Organisedby: PaulO'Brien(LeicesterUniversity), StephenSmartt(QueensUni-versityBelfast), JonathanGranot(UniversityofHertfordshire), NialTanvir (Le-icesterUniversity)
15:45 JonathanGranot: Highlights fromFermiobservationsofGamma-RayBursts
16:30 MassimilianoDePasquale: GRB090510, thefirstcasestudyofashortGRB withGeV extendedemissiondetectedbyFermiandSwift.
16:45 AntoniaRowlinson: DiscoveryoftheafterglowandhostgalaxyofthelowredshiftshortGRB 080905A
17:00 RachelTunnicliffe: InvestigationoftheenvironmentofshortgammarayburstGRB090510withaviewtoconstrainingtheprojenitor.
17:15 TomMuxlow: Discoveryofanunusualnewradiosourceinthestar-forminggalaxyM82: Faintsupernova, supermassiveblackhole, oranextra-galacticmicroquasar?
Posters LauraWatson: FindingtheSourceofUHECRsusingBayesianAnalysisofPierreAugerData
P26 TheSloanDigitalSkySurvey: theLegacyandFuture [2010April15, 10:45, p76]
TheSloanDigitalSkySurvey (SDSS) is themostproductive surveyof the sky(Madrid&Macchero2009), withover65 thousandcitations to theSDSS viaADS.Inthissession, wewillgiveanoverviewoftheoutstandingSDSS discover-iessincefirstlightadecadeago, whilealsolookingforwardtothenewSDSS-III(www.sdss3.org)projectwhichcontinuesthislegacy. Thesessionwillcoveradiverserangeofscience(planetstodarkenergy)andtopics(dataaccesstopub-licationissues).
Organisedby: BobNichol(ICG,Portsmouth)
10:45 IvanBaldry: Globalpopulationstatistics, bimodalityandmultivariatedistributionsofgalaxieswithSDSS.
11:03 NicholasRoss: TheSDSS-III BaryonOscillationSpectroscopicSurvey(BOSS):FirstResults
11:21 MathewSmith: SDSS-II SNe-AnOverviewandHostGalaxyProperties
11:39 JonLoveday: GalaxyClusteringintheSDSS
11:57 CristianoSabiu: Higher-OrderClusteringOfLuminousRedGalaxiesInTheSDSS
12:04 BorisGaensicke: Whitedwarfsastracersofstellar, binary, andplane-taryevolution
12:11 ZengHuaZhang: Discoveryof thefirstwideL dwarf+giantbinarysystemandeightotherultra-cooldwarfsinwidebinaries
12:18 AshleyRoss: AnalysingtheClusteringofPhotometricallySelectedGalax-ies
12:25 AvonHuxor: EvidenceofTidalStrippingofthreecompactelliptical(cE)galaxiesdiscoveredinSDSS DR7
Posters DavidMurphy: DVORACDetector-TheDurhamVOronoiRed-sequenceAutomatedClusterDetectorfornext-generationpanoramicsurveys
31
LiekevanSpaandonk: BinarypopulationsinSDSS:A newdiagnosticforsystemparametersofevolvedwhitedwarfbinaries
P27 StellarPopulationsinGalaxies [2010April15, 10:45, p78]
Thestudyofstellarpopulationsprovidesvitalcluesontheevolutionofgalaxiesandtheunderlyingphysicalprocesses. Theinterpretationofphotometricandspectroscopicdatafromresolvedandunresolvedstellarsystemsrestsontheac-curacyofstellarevolutionmodelsandmodelatmospheres, theircombinationintopopulationsynthesismodels, andthetechniquesemployedtofittheorytoobservations.
Thegoalofthissessionistodiscussourcurrentknowledgeofresolvedandunre-solvedstellarpopulations, focusingonboththedifferencesamongmodelsandmethodsweemploy inouranalyses, and thedevelopmentsnecessary for thefullexploitationofdatafromthecurrent-andnext-generationofastronomicalfacilities.
Organisedby: MaurizioSalaris(LiverpoolJohnMooresUniversity)
10:45 RussellSmith: Learningaboutstellarpopulationsinunresolvedgalaxies
11:05 SusanPercival: Systematicuncertaintiesinherentinstellarpopulationsynthesismodelsandtheirimpactonintegratedspectraofstellarpop-ulations: A modeller'sperspective.
11:20 JohnEldridge: BPASS:BinaryPopulationandSpectralSynthesis
11:35 SugataKaviraj: Theroleofminormergersinthestarformationhistoryofearly-typegalaxies
11:50 IgnacioFerreras: ConstrainingtheInitialMassFunction
12:05 MichaelBarker: TheLastMajorEpochofDiskGrowthinM3312:20 Posteradverts
Posters RichardHutcheon: KinematicbiasinexoplanetsurveysOliviaJones: Crystallinesilicatesaroundoxygen-richAsymptoticGiantBranchStarsintheLargeMagellanicCloud
LisetteSibbons: TheAGB populationand themetallicitygradient inNGC 6822
BejaminTatton: AGB StarsinWLMPaulWoods: ThestellarpopulationsintheLargeMagellanicCloud
P28 GeneralMIST ScienceSession2 [2010April15, 10:45, p79]
Magnetospheric-Ionospheric-Solar-Terrestrial(MIST) researchconcernsphysicalprocesseswithintheSun-Earthsystem, othersolarsystembodiesandexo-planets;inparticularthesolar/stellarwind, moonsandplanetaryatmospheresandmag-netospheres. TheMIST generalsessionisdesignedtoaddressthoseaspectsofcurrentMIST researchnotexplicitlycoveredinothersessions, suchasneutralat-mospherescience, ULF wavesandwave-particleinteractions, auroralandiono-sphericelectrodynamics, andground-basedstudiesofthecoupledmagnetosphere-ionosphere system. All researcherswhoare interested inanyaspectofMISTsciencearethereforeinvitedtotakepart.
Organisedby: AdrianGrocott(UniversityofLeicester), EmmaWoodfield(Uni-versityofLancaster), AndrewFazakerley(UniversityCollege, London, MSSL)
10:45 TimothySpain: SCANDI:All-skyviewofmeso-scalespatialstructureinthethermosphereandion-neutralcouplingoverSvalbard
11:05 AndrewSenior: ObservationsandmodellingofartificialD-regionheat-ingseenbyARIES
32
11:20 HannahVickers: Observationsofdouble-peakedHF radarspectraduetomixedechoesfromnaturalandartificialplasmairregularities
11:35 SheilaKanani: Overviewof lowenergyelectronobservations in thevicinityofSaturn'smoonEnceladus
11:50 GabbyProvan: Evidencefortheoccurrenceof 10.6hmagneticfieldoscillationsinSaturn’sequatorialmagnetosphere
12:05 DavidAndrews: Magnetospheric-periodoscillationsinSaturn'sequa-torialmagnetosphereandopentaillobesthroughouttheCassinimis-sion
12:20 PosteradvertsPosters Ciaran Beggan: Interpolation of external magnetic fields over large
sparsearraysusingSphericalElementaryCurrentSystemsEllenClarke: AnestimationoftheCarringtonflaremagnitudefromsolarflareeffects(sfe)inthegeomagneticrecordsAdrianGrocott: SuperDARN observationsofthesub-auroralconvec-tionresponsetoenhancedgeomagneticactivityJohnHargreaves: ThedriftofauroralradioabsorptionpatchesobservedbyimagingriometerStephanieKellett: NatureoftheringcurrentinSaturn’sdaysidemagne-tosphereGemmaKelly: TowardsmodellingofhighlatitudemagneticfieldsfromsatellitedataAnthonyWilliams: TrackingsolarwindstructuresfromtheSunthroughtotheorbitofMarsEmmaWoodfield: CombiningincoherentscatterradardataandIRI2007tomonitortheopen-closedfieldlineboundaryduringsubstorms.
P29 ModellingofDynamicSolarPlasmas [2010April15, 10:45,p79]
Newspacemissionswiththeirhigherspatial, spectral, andinparticulartemporalresolutionareprovidingapictureofamoredynamicsolaratmosphere. Suchobservationsrequireatime-dependentmodellingapproach. Whatisthestatusofcurrentmodellingasregardstransientionization? Wheredowestandregardinghydrodynamicandmagneto-hydrodynamicmodellingoftheconstantlychangingsolaratmosphereonsmallscales? Thissessionwillbelargelydirectedtowardsthemodellingofvariousdynamic featureswhetherobservedfromthegroundorspacebasedinstruments. ItwillbringtogethernotonlyMHD andHD expertsbutitwillalsodiscussvariousaspectsofthepresentmodellingrelatingtoatomicphysics.
Organisedby: GerryDoyle(ArmaghObservatory), MariaMadjarska(ArmaghObservatory)10:45 MariaMadjarska: PlasmapropertiesofanX-rayjetfrommulti-instrument
co-observations: SUMER/SoHO,EIS/XRT/HinodeandEUVI/SECCHI/STEREOA andB
11:00 PeterCargill: A newenthalpy-basedapproachtothetransitionregioninanimpulsively-heatedcorona
11:15 JiaoyangDing: Chromosphericmagnetic reconnection: implicationsforjet-likeeventsandcoronalheating
11:30 DavidTsiklauri: TheHydrodynamicEvolutionofImpulsivelyHeatedCoronalLoops: ExplicitAnalyticalApproximations
11:45 KarenMeyer: Non-LinearForce-FreeModeloftheSolarMagneticCar-pet
12:00 UrmilaMitraKraev: Detailedobservationsandmodellingofasmallflare
33
12:15 HughPotts: Theopticaldepthofwhite-lightflarecontinuumPosters ZhenghuaHuang: Observationand3D modellingofacoronalbright
pointGuiyunLiang: CalculationandapplicationofR-matrixelectron-impactexcitationdataforionsofinteresttoastrophysicaldiagnosticmodellingProchetaMallik: AlfvénIonisationintheSolarPhotosphereSrividyaSubramanian: Whatblinkersactuallyare?KamalamVanninathan: SpiculesandCoronalHeatingLidiavanDriel-Gesztelyi: MagneticreconnectionalongQSLs-amajordriverofactiveregionoutflows
P30 PulsarAstrophysics [2010April15, 10:45, p81]
More than40yearsafter theirdiscovery, pulsars (and latterly, magnetars) stillpresentextraordinarychallengestoastrophysicalmodellinganddataanalysis.Progressisbeingmadeinunderstandingtheunderlyingphysicsthatgovernstheemissioncharacteristicsof theseextraordinaryobjects, butmuch remainsun-clearorunknown. Thephysicsoftheinterior, thecrustandtheatmosphereofneutronstarsrequireustoconfrontourunderstandingofthebehaviourofmat-terandradiationinextremeconditions. Thereisawealthofobservationaldata,andadiversityofapplicationforthisdata, thatmakesaclearercomprehensionofemissionprocessesandimplicationsallthemoreurgent. Weinvitesubmis-sionsfromallthoseinterestedpartieswhoareaddressingthefollowingtopicsintheirresearch: neutronstarinteriors; neutronstarcrusts; neutronstaratmo-spheres; pulsarplasmasandradiationmechanisms; behaviourofmatterunderextrememagneticandgravitationalfields; ultra-energeticprocessesinthepulsarenvironment; physicalinterpretationofradiationcharacteristicsofpulsarsandmagnetars.
Organisedby: NilsAndersson(UniversityofSouthampton), DeclanDiver(Uni-versityofGlasgow), AntoniodaCosta(InstitutoSuperiorTecnico-UTL,Lisbon)10:45 IntroductoryoverviewbyDonMelrose11:05 AntonioArmandodaCosta: PulsarElectrodynamics: TheRelativistic
KineticTheoryofRadiativePlasmas—TheGamma-raycut-off11:15 CristobalEspinoza: GlitchesintherotationofPulsars11:25 RobertFerdman: Testsofgeneralrelativityandbinaryevolutionstudies
usingpulsarobservations11:35 IkSiongHeng: A BayesianSearchForGravitationalWaveRing-downs
AssociatedWithPulsarGlitches11:45 WynnHo: CarbonatmosphereneutronstarinCassiopeiaA:Youngest
neutronstarintheGalaxy11:55 DominicKeogh: LatestHESS observationsofPulsarWindNebulae12:05 AndrewLevan: TheopticalandinfraredcounterpartofSGR 0501+451612:15 DeclanDiver: SurfaceextractionofelectronsinapulsarPosters EwanBarr: TheEffelsbergNorthernSkyPulsarSurvey
MatthewPitkin: KnownpulsarsascontinuousgravitationalwavesourcesSatoruSakai: TheeffectofGravitationalDistortionof SpacetimeonPulsarTimingNeilYoung: IntermittentRadioEmissionfromPSR B0823+26
P31 TheRoleofFeedbackinGalaxyEvolution [2010April16,10:45, p82]
Feedbackprocesses, bothfromsupernovaeandAGN,arebelievedtobeanim-portantprocessinshapingthegalaxyluminosityfunction, withdifferentmecha-
34
nismsbeingimportantatdifferentmassscales. Thissessionwilladdressfeedbackfrombothobservationalandtheoreticalperspectivesandinvestigatetheenerget-icsoftheprocessesatwork. MechanismsforthetriggeringandterminationofstarformationandAGN activitywillbeexplored.
Organisedby: ChrisSimpson(LiverpoolJohnMooresUniversity)10:45 SarahBryan: The impactof feedbackon theorbital contentofdark
matterhaloes.11:00 ElisaHouse: DiskHeating: ComparingtheMilkyWaywithCosmolog-
icalSimulations11:15 SamGeen: TheroleoffeedbackinMilkyWaysatellitegalaxyformation
usinghighresolutionsimulations11:30 GregStinson: StellarFeedbackinSPH GalaxyFormationSimulations11:45 MarkWestmoquette: Superstarclusterfeedbackfromlocaltogalaxy
scales12:00 JamesFalder: TheEnviromentsofAGN atz 112:15 AsaBluck: TheCo-EvolutionofMassiveGalaxiesandtheirSupermas-
siveBlackHolesoverthelast11.5GyrsPosters EmilyDown: Theorientationofaccretiondisksandjetsinquasars
KathrynHarris: ClusterandGalaxyEnvironmentsofQuasarsElizabethMannering: TheMulti-facetedX-rayactivityofthecomplete3CRR AGN sampleatz<0.1RachaelMcQuillin: MomentumdrivenfeedbackfromstellarnucleiKatePilkington: TheColdGasContentofBulgelessDiskGalaxiesCyprianRangel: SearchingforComptonThickAGN atz 2indeepX-rayfieldsXufenWu: StabilityandevolutionofclustergalaxiesinMOND
P32 StellarandExoplanetaryMagnetism [2010April16, 10:45,p84]
Thepastfewyearshaveseenthedetectionofmagneticstar-planetinteraction(SPI),anewlydiscoveredphenomenonthatmayyieldamethodofcharacteris-ingexoplanetarymagneticfieldsandconsequentlytheirinternalstructure. TheexistenceofmagneticSPI remainscontroversial, however, ifconfirmed, itwouldallowour Solar System tobeplaced in contextwith other planetary systemswithintheGalaxy. Asforstellarmagnetism, recentdiscoveriesincludethepos-sibledetectionofaremnantfossilfieldonahotmassivestar; thefirsteversurfacemapsofpre-mainsequencestarsintheclassicalT Tauriphaseoftheirevolution;thediscoveryofamagneticcycleonastarpossiblyinducedbyaknownorbit-ingclose-ingiantplanet; therapidincreaseinfieldcomplexityatthetransitionfromcompletelyconvectivelow-massstarstothosewithradiativecores; andthediscoveryofgloballystructuredmagneticfieldsontheintermediatemassHerbigAe-Bestars. Thissessionwillhighlight thelatestresults inthestudyofstellarmagnetismacrosstheHR diagram, andexoplanetarysystems.
Organisedby: ScottGregory(UniversityofExeter)10:45 GaiteeHussain: Stellarmagnetisminsolar-typestars11:15 RobJeffries: MagneticactivityinfastrotatingM-dwarfsaboveandbe-
lowthefullyconvectiveboundary11:30 StefanoBagnulo: StellarmagnetismthroughtheeyesoftheFORS1in-
strumentoftheESO VLT12:00 AlineVidotto: Theinfluenceofthestellarwindonclose-ingiantplanets12:15 GrantMiller: TheDopplerShadowofWASP-3bPosters RobertDeRosa: InvestigatingtheX-rayEmissionofA-typeStarsThrough
theMagneticActivityofUnresolvedLowerMassCompanions
35
ScottGregory: Testingtheabilityoffieldextrapolationmodelstopre-dicttheX-raypropertiesofpre-mainsequencestars
P33 PublicEngagementinAstronomy, SolarandSolarSystemPhysics [2010April16, 10:45, p85]
Overthepasttwoyears, publicengagementandoutreachinAstronomy, SolarandSolarTerrestrialPhysicsintheUK hasgainedmomentumduetotheInter-nationalHeliophysicalYear(IHY) andtheInternationalYearofAstronomy(IYA).
Inthissession, wewanttoexplorethenewopportunitiesthathavebeenopenedupbythesetwoprogrammes, hearingfromthepeoplewholedtheseinitiativesandotherswhoransuccessfulevents. SinceboththeIHY andIYA havenowfinished, it is timely todiscusswhathasbeensuccessfulaboutbothoutreachprogrammes, enablethoseinterestedinoutreachtodiscussbestpractice–andalsohow to retain themomentumand takeoutreach in theUK further. Thesessionwillcontainthefollowing:
• ReviewtalksfromanIHY andanIYA organisertosummarisethesuccessesoftheinternationalyears(20minseach);
• Contributedtalksfromthosewhoactivelyparticipatedinoutreachactivi-tiesduringIHY andIYA.Sharingofexperiencesandinsights;
• 'Speednetworking'–likespeeddating, butwiththeemphasisonnetwork-ingwithotherpeopleinterestedinoutreach;
• Discussion–generaldiscussion, howcanwesharebestpracticeacrossAstronomy, Solar&STP?HowdomaintainthemomentumforoutreachfromtheIHY andIYA?Howimportantinoutreachinthegrantsthatweapplyfor? Whatcountsasoutreachandwhatdoesn't?
Organisedby: DanHillier(ROE VisitorCentre), HelenMason(DAMTP,Cam-bridge), DanielleBewsher(UniversityofCentralLancashire)
10:45 Introductoryremarks
10:50 SteveOwens: BeyondIYA2009: SustainableScienceEngagement
11:00 LucieGreen: OutreachduringInternationalHeliophysicalYear
11:10 AlecMacKinnon: SchoolsoutreachfortheGlasgowNAM
11:15 IngeHeyer: IYA 2009ontheBigIslandofHawaii
11:20 OliviaJohnson: Beyondconstellationstories: communicatingcutting-edgescienceandengagingnewaudiencesthroughnovelplanetariumprogrammingfortheInternationalYearofAstronomy
11:25 HelenWalker: TheSocietyforPopularAstronomy'sTelescopesforSchoolsProject
11:30 DanHillier: UK DarkSkyDiscovery
11:35 CharlesBarclay: Astronomyinthecurriculum. DevelopmentsatKS4andKS5
11:40 AlisonWallace: Challenges of Public EngagementwithChildren inCare
11:45 HelenMason: Sun|trek-thefinalfrontier
11:50 JimWild: DidtheSunEarthPlanworkout?
11:55 DanielleBewsher: TheBigBang!
12:00 Discussion/soapbox
Posters MartinHendry: TheScottishSolarSystem
MartinHendry: DevelopmentofanAll-SkyCameraforOutreachAc-tivities
36
DonaldKurtz: SongsoftheStars: theRealMusicoftheSpheres
StuartLowe: 4YearsofPodcasting
RichardMorton: TheMusicoftheSunasaStar
P34 UKSP GeneralSession [2010April16, 10:45, p87]
Thissessionisdesignedtoaddressthecurrentsolarresearchnotcoveredinothersessions. Allresearcherswhoareinterestedinsolarphysicsareinvitedtotakepart.
Organisedby: DuncanMackay(UniversityofStAndrews), BarbaraBromage(UniversityofCentralLancashire), RekhaJain(UniversityofSheffield), EduardKontar(UniversityofGlasgow)
10:45 PaulHiggins: TheMagneticPropertiesofFlaringActiveRegions
11:00 NicolasLabrosse: NewsolarprominencediagnosticswithEIS/Hinode
11:15 JenniferHarris: Largeamplitudetransverseoscillationsinamulti-strandedEUV prominence, triggeredbytransientdisturbances
11:30 JamesMcLaughlin: Phasemixingofnon-linearAlfvénwaves
11:45 JamesThrelfall: Alfvénwavephase-mixinganddampingintheioncy-clotronrangeoffrequencies
12:00 FraserWatson: Automated detection and tracking ofmagnetic frag-mentsindecayingsolaractiveregions
12:15 DavidMacTaggart: Simulationsofmagneticfluxemergencewithanoverlyingfield
Posters VasilisArchontis: MagneticfluxemergenceandcoronaleruptionsintheSun
MarioBisi: Medium-andsmall-scaletransientsinthesolarwind
BarbaraBromage: AnomalousSolarCyclesandtheEvolutionofCoro-nalHoles
KenDere: ChiantiPy-A PythonInterfacetoCHIANTI
GarethDorrian: RapidOscillationsintheSolarAtmosphere
EduardKontar: HardX-RayStructureofLoopFootpointsinaSolarLimbFlare
XingLi: KineticAlfvénwavesandprotonvelocitydistributionin thesolarwind
BrendanO'Dwyer: SDO/AIA responsetocoronalhole, quietsun, ac-tiveregionandflareplasma
P35 NewTechnologiesforFutureInstruments, TelescopesandMissions [2010April16, 10:45, p89]
TheUK hasalongstandingheritageindevelopingthekeytechnologiesforsomeofthemostsuccessfulandstate-of-the-artinstruments, telescopesandmissionsforastronomy. Thenextgenerationofrequirementsposessomenewchallenges,and in thecurrentandnear-termeconomicclimate thecommunitywillmostlikelyhavetobemoreselectiveinidentifyingtheareaswhereourskillsarebestsuited. WhatarethenewtechnologiestheUK shouldbefocussinguponoverthenext10+years? Thesemayinclude, butarenotlimitedto, advanceddetec-torsandreadouts, novelnewlightweightsupportstructuresforspacetelescopes,portablehigh-coolingpower systems, highly reflectiveor transmissiveopticalcomponents, low-lossmaterialsforroomtemperatureandcryogenicoperation,newideasforactiveandadpativecontrolsystems, etc. Whilstmuchofthenear-tomid-termislikelytoconcentrateonE-ELT,SKA and2ndgenerationgravita-tionalwavetelescopeswemustalsonotlosetrackofmissionsthatarepotentially
37
furtherdownstream(e.g. spaceinterferometrysuchasFIRI andtheEinsteintele-scope). Thissessioninvitestalksandpostersfromastronomers, physicistsandengineers, withinbothacademiaandindustry, onanytechnologydevelopmentareasthatmightbenefitthemissionsofthefuture.
Organisedby: WayneHolland(UK ATC,Edinburgh), GilesHammond(Univer-sityofGlasgow), DaveMelotte(UK ATC,Edinburgh)
10:45 FraserClarke: HARMONI -A UK ledfirst light spectrograph for theE-ELT
11:00 SimonDoyle: LumpedElementKineticInductanceDetectorssuitableforlargearraysofastronomicaldetectors.
11:15 MelStrachan: Noveldeformablemirrordevelopmentsforastronomyapplications
11:30 StefanHild: High-PrecisionInterferometryandLow-LossmaterialsforfutureGravitationalWaveObservatories
11:45 IanHepburn: Milli-kelvincoolerfortheXMS instrumentontheInter-nationalX-rayObservatory
12:00 NicolaBeveridge: Hydroxidecatalysisbondingresearchforastronom-icalapplications
12:15 JanBergman: FIRST Explorer-spacebornelow-frequencyradioastron-omyusingpassiveformationflying
Posters JuliaKennedy: Reducingriskincryogenicinstrumentdesign: thermalconductivitymeasurementsattheCryogenicInstrumentationResearchLab
GiovannaTinetti: Probingtheatmospheresofextrasolarworldswithadedicatedmissionfromspace
RichardWhite: Astronomyatthehighestenergies: theCherenkovTele-scopeArray
38
39
RA
SA
ftern
oon Session1: 14:00–15:20
WelcomefromRAS President, ProfessorAndyFabian.
Thefollowingmedalsandprizeswillbepresented. ThecitationsofmedalsandprizeswillbereadbyDrFionaSpeiritsandFraserWatson.
TheGoldMedalforGeophysics ProfessorJohnWoodhouseFRSUniversityofOxford
TheHerschelMedal ProfessorJamesHoughUniversityofHertfordshire
TheChapmanMedal ProfessorBernardRobertsUniversityofSt.Andrews
TheJackson-GwiltMedal DrCraigD MackayUniversityofCambridge
AwardForServiceToAstronomy ProfessorFranciscoSanchezInstituteofAstrophysicsoftheCanaryIslands
AwardForServiceToGeophysics DrFrankLowesUniversityofNewcastleuponTyne
GroupAchievementAwardForAstronomy SuperWASP teamrepresentedbyProfessorDonPollacco, Queen'sUniversity, Belfast
GroupAchievementAwardForGeophysics CHIANTI consortiumrepresentedbyProfessorKenDere, GeorgeMasonUniversity, Virginia
HonoraryFellowship ProfessorConnyAertsUniversityofLeuvenandRadboudUniversity, Nijmegen
HonoraryFellowship DrWlodekKofmanTheLaboratoryforPlanetology, Grenoble
TheFowlerAwardForAstronomy DrBarbaraErcolanoUniversityofCambridge
WintonCapitalAwardForAstronomy DrElizabethStanwayUniversityofBristol
WintonCapitalAwardForGeophysics DrDavidRobinsonUniversityofOxford
Thefollowingprizewinnerswereunabletoattend.
TheGoldMedalforAstronomy ProfessorDouglasGoughUniversityofCambridge
TheFowlerPrizeforGeophysics DrInekedeMoortelUniversityofStAndrews
ProfessorCarlosFrenkwillgivetheDarwin2010Lectureon‘Thestandardmodelofcosmogony: whatnext?’
Session2: 15:45–17:30
The futureofUK astronomy–adiscussionchairedbyProfessorAndyFabian(PresidentoftheAstronomyForum), includingpresentationsanddiscussionontheUK SpaceAgency, STFC andthe2011ComprehensiveSpendingReview. TheparticipantswillincluderepresentativesofSTFC andotheragencies.
41
Abs
tract
s LifeonTitanWilliamBains (RufusScientific/MIT)
Livingthingshavedistinctcharacteristicsthatconstraintheirpossiblechemistry, andhencewhereandhowwemightlookforthem. I willdiscusstheexampleofTitan: couldtherebelifeonthesurface? Majorlimitationsarethestability,solubilityandreactivityofthechemicalsthatmakeuplife, andenergysourcestodrivemetabolism. Iwillreviewhowtheseconstraintscanbeusedtoputlimitsonwherelifemightoccur, andthebiochemistrythatwemightlookforeitherremotelyorwhenwegetthere. ThesurfaceofTitandoesnotlookpromising, butifthereislifethereitwillbesimple, explosivelyunstableunderEarthconditions, and(tous)extremelysmelly.
TheSuperWASP ProjectAndrewCameron (UniversityofStAndrews)with
D. Pollacco, C. Hellier, R. West, and WASPConsortium
TheWASP consortiumiscurrentlytheworld'sleadingproducerofextra-solarplanetstransitingbrightstars. Itstwoautomatedwide-fieldcameraarrays, SuperWASP onLaPalmaandWASP-SouthatSutherland, eachimagesome15percentoftheskywithacadenceof7to8minutesforbetween4and8hourseachnight. Automatedsoftwareidentifiesstarsexhibitingtheone-percentdipsinlight, recurringeveryfewdays, thatbetraythepresenceofacompactsub- stellarcompanion.Efficientwinnowingoflikelycandidatesforradial-velocityfollowup, incollaborationwiththeGenevaandIAP/Haute-Provenceplanetsearchteams, hasledtothediscoveryofsome30transitingplanetstodate. InthispresentationI willannounceanumberofnewlyconfirmedWASPplanets. WASP'spublishedplanetdiscoveriesareenrichingourunderstandingoftheclosest-orbitinggasgiantplanetsaroundotherstars. Theyincludethehottest, mostinflatedandshortestperiodplanetsyetidentified. Manyhaverelativelymundanecircularorbitsinthestellarequatorialplane. Othershavehighlydisturbedeccentric,inclinedandevenretrogradeorbits. Theyrevealarichsetofplanetaryformationandmigrationhistories. Somearegrosslyinflatedbyacombinationofextremeirradiationandtidalenergydissipation. A smallnumberorbitsoclosetotheirstarsthattidalorbitdecaywillleadtotheirdestructionwithinthemain-sequencelifetimesoftheirhoststars. Aboveall, theWASP systemsarebright. TheirdaysidethermalradiationisaccessibletoSPITZER andhasevenbeendetectedfromtheground, revealingawealthofinformationabouttheiratmosphericthermalstructureandchemistry. I willpreviewthefirstpublicreleaseofprocessedlightcurvedatafromtheinitialyearoftheWASP project, whichwilltakeplacethisyear.
DesignchallengesintheconstructionofELTsColinCunningham (UK AstronomyTechnology
Centre)
TheEuropeanExtremelyLargeTelescopeisreachingcompletionofitsdesignphase. Likeanymajorproject, ithastobalancecost, riskandperformanceinordertobeaffordableonacompetitivetime-scaleandbeabletosatisfyambitioussciencegoals. I willdescribehowthisbalancehasbeenachievedwhilstmaintainingtheaspirationtobuildtheworld'slargestoptical/IRtelescopewithbuiltinadaptiveoptics. I willemphasizeUK rolesinaddressingtheconsiderablechallengesofdevelopingtheprimarymirrorconsistingof984segments, theadaptiveoptics
systems, andtheinstrumentsuite. Finally, I willshowsomeoftheexcitingprospectsforscientific,technologicalandindustrialbenefitstotheUK.
ProbingCosmologywiththeCMBRGeorgeEfstathiou (KavliInstituteforCosmology)
ThePlanckMissionwaslaunchedsuccessfullyinMaylastyear. I willgiveasummaryofthescientificaimsofthePlanckMissionandabriefoverviewofitscurrentstatus. I willalsoplacethePlanckmissionincontextwithgroundandsuborbitalCMB experimentsandotherprobesofearlyuniversecosmology.
TheEarlyStagesofStarFormationJenniferHatchell (UniversityofExeter)
Wheredostarsform? Howlongdoesittake?Whatcontrolstheirmasses? Thesequestionsandmorearebeingaddressedbymappingsurveysofmolecularcloudsatlongwavelengths(infraredandsubmillimetre), whichprovideacensusofdensecoresandthestarsformingwithinthem. Iwillshowhowtheadvancesintechnologywhichallowustomaplargeareasaremirroredinourincreasedunderstandingoftheearly, embeddedstagesofstarformation, andlooktowardsthefuturewithHerschelandSCUBA2.
TheHighEnergySunBobLin (Univ. ofCalifornia, Berkeley)
TheSunisthemostprolificandenergeticnaturalparticleacceleratorinthesolarsystem. Largesolarflaresarethemostpowerfulexplosionsinthesolarsystem, releasingupto ∼ 1032-33ergsin100-1000s, with &10-50%ofthisenergygoingtoacceleratingelectronsto ∼ 20 keV to ∼ 100sofMeV,andacomparableamounttoacceleratingionsto ∼ MeV to GeV energies. ImagingbytheRHESSI (RamatyHighResolutionSolarSpectroscopicImager)spacecraftofthehardX-ray(HXR)/γ−raycontinuumand γ−raylineemissionproducedbytheacceleratedelectronsandions,respectively, showthattheprocessofmagneticreconnectionunderliesboththeflareenergyreleaseandtheaccelerationofelectronsandions.InlargeSolarEnergeticParticles(SEP) events, ionsupto ∼ 100 GeV andelectronsupto ∼ 10sofMeV,wellintothegalacticcosmicrayenergyrange, aredetectedinsitunear1AU.Theseappeartobeacceleratedbycollisionlessshockwavesdrivenbyfast(&1000km/s)coronalmassejections(CMEs)withoforder ∼ 10 %ofthetotalCME energygoingintotheSEPs, thesameefficiencyasrequiredforsupernovashockstoaccelerategalacticcosmicrays. Themostcommon(&100s/monthnearsolarmaximum)solaraccelerationoccurshighinthecoronaandproducestheimpulsiveSEP eventsobservedintheinterplanetarymedium, thataredominatedby∼ 0.1 − 100 keV electronsandby ∼ 10 keV toMeV pernucleonionswithenormous(upto&10,000)enrichmentsintheisotope3Heandinultraheavyelements. Theaccelerationmechanismsare, atbest, poorlyunderstood;upcomingmissionsgoingclosetotheSun, suchasESA’sSolarOrbiter(∼ 0.28 AU) andNASA’sSolarProbePlus(∼ 9.5 solarradii), promisetoprovidekeyrelevantmeasurements.
TheESA CosmicVisionProgrammeMarkMcCaughrean (ESA)
I willpresentabriefoverviewoftheESA spacescienceandroboticexplorationprogramme,
42 Plenary
coveringmissionscurrentlyinoperation(includingHerschel, Planck, andRosetta)andthoseinpreparation(LISA Pathfinder, Gaia, JWST,BepiColombo, andtheExoMarsmissions). ThemajorityofmytalkwillconcentrateonthestatusandpromiseofthemissionscurrentlyunderstudyaspartoftheCosmicVisionprogramme, andtheroadmapfornewopportunitiesoverthecomingdecade.
PlasmaphenomenaonallcosmicscalesDonMelrose (UniversityofSydney)
I willgiveabriefhistoricalreviewofthedevelopmentofthefieldofplasmaastrophysics,emphasizingtheproblemsthatmotivatedthefield,andthenewplasma-physicsideasthatwereintroducedtoaddresstheseproblems. I willthendiscussthepresent-daystatusofthreegenericproblemsinplasmaastrophysics: 1. resonantscatteringandparticleacceleration; 2. coherentradioemissionmechanisms; and3. dissipationincollisionlessastrophysicalplasmas.
Proto-planetarydisksandplanetarymigrationRichardNelson (QueenMary, Universityof
London)
Thediscoveryofextrasolarplanetswithawiderangeoforbitalconfigurationssuggeststhatorbitalmigrationplaysafundamentalroleduringtheformationofplanetarysystems. DuringthetalkIwillreviewourcurrentunderstandingofplanetarymigration, anditsdependenceonthephysicalpropertiesofprotoplanetarydiscs, withtheroleofdiscthermodynamicsandturbulencebeinghighlighted. Modelsofplanetarysystemformationincludingmigrationwillbepresented.
GravitationalAstronomyBangaloreSathyaprakash (CardiffUniversity)
ThefirstdirectdetectionofgravitationalwavesareexpectedwithinthenextfivetosixyearswhenadvancedLIGO andVirgodetectorsbegintooperate. Thefirstdetection, whilealandmark, isonlythebeginningofwhatpromisestobeanewtoolforobservationalastronomy, cosmologyandfundamentalphysics. InmytalkI willdiscussthecurrentstatusofgravitational-waveobservationsandcapabilitiesoffuturedetectors. I willshowhowfutureobservationsmightimpactourunderstandingofastrophysicalphenomena(e.g.,neutronstars, blackholes, supernovae, GRGs),fundamentalphysics(e.g., matterunderextremeconditions, strong-fieldtestsofGR,darkenergy)andcosmology(e.g., cosmologicalparameters,blackholeseeds, stochasticbackgroundsfromtheearlyUniverse).
ExploringtheUniversewithGamma-RayburstsNialTanvir (UniversityofLeicester)
Thankstotheirextraordinaryluminosities, γ−rayburstscanbeseenatveryhighredshifts, andassuchprovidepowerfultoolsforexploringearlystructureformationandreionization.Spectroscopyoftheirafterglowsgivesredshifts,andpotentiallyalsoinformationaboutchemicalenrichmentoftheirhostsandthestateoftheintergalactic-mediumclosetotheburst.Identificationandcharacterisationoftheirfainthostsandneighbouringgalaxiesopensanewwindowongalaxyevolution. RecentlyGRB090423wasdetectedatredshiftz=8.2,highlightingthepromiseofGRBsforprobingtheveryhighredshiftuniverse. I willreviewthiswork
andotherrecentdevelopmentsinthefield,includingthestatusofhostgalaxysearches.
TheSWARM MissionKathyWhaler (UniversityofEdinburgh)
In1999, theInternationalUnionofGeodesyandGeophysicsadoptedaresolutiontoestablishanInternationalDecadeofGeopotentialFieldResearch, heraldingthestartofadecadeofcontinuousmonitoringofthemagneticfieldbynear-Earthorbitingsatellites, andimportantadvancesinspace-basedgravityfieldobservation.FormuchoftheInternationalDecade, multi-satellitevectormagneticobservationshavebeenavailable, leadingtomuchbettermodelsofthemainfieldanditsrateofchange, andimprovedunderstandingoftheinfluenceofmagnetosphericandionosphericfieldsonattemptstoisolatetheinternalfieldsignal. However, muchremainstobedone. Forinstance, evenduringtheparticularlyquietsolaractivityconditionsthathavecharacterisedmuchofthelastfewyears, andafterenormouseffortondataprocessingandselectionalgorithms, magnetosphericandionosphericfieldeffectsremainindatausedtoproduceinternalfieldmodels, sooursignalidentificationandseparationisfarfromperfect; 'comprehensivemodels'thatareintendedtoparameteriseandmodelknowninternalfieldsourcesandmagnetospheric/ionosphericcurrentsystemsarestillonlyappropriateformagneticallyquiettimes.However, thedemonstratedpowerfromhavingavailablesimultaneousmulti-satelliteinformationhasledtoESA approvalforasatelliteconstellationSWARM withintheEarthExplorerprogramme,scheduledforlaunchin2011. Inthistalk, I willdescribetheSWARM missiondevelopmentandanticipatedapplicationsofthedata, includinghowtheend-to-endsimulatorstudywasusedtoimprovetheconstellationdesignoverthatintheoriginalproposal, andthepotentialofSWARM forinvestigatingatmosphericprocessesrelatedtoclimateandweather, suchasspaceweatherandradiationhazards, aswellasthebetterdefinitionofthe'geological'magneticfieldsignalandnear-Earthexternalmagneticfields.
TheJamesWebbSpaceTelescopeGillianWright (UniversityofEdinburgh)
TheJamesWebbSpaceTelescope(JWST),thesuccessortoHubble, isalarge, 6.5mdiameter,infrared-optimizedspacetelescope, scheduledforlaunchin2014. ItwillhaveasuiteoffourinstrumentsdesignedtoenablewiderangingsciencefromthefirstluminousgalaxiesandgalaxyevolutiontotheformationofplanetsandtheevolutionofourownSolarSystem. InthistalkI describethesciencethemesthathavedriventheobservatorydesign, theenablingtechnologiesandtechnicalstatusofthemissionandtheinstrumentcapabilities, inparticularforthemid-infraredinstrumentMIRI.I willalsosummarisetheplansforoperations.
GalaxiesandStellarPopulationsRosieWyse (JohnsHopkinsUniversity)
I willdiscusshowstudyingresolvedstarsinthenearbyUniversecanbeusedtoinferconditionsathighredshift, tracehowgalaxiesevolveandconstrainthenatureofdarkmatter. Thisapproachiscomplementarytodirectstudyofsystemsathighredshift, butI willshowthatanalysisofindividualstarsallowsonetobreakdegeneracies,suchasbetweenstarformationrateandstellar
InitialMassFunction, thatcomplicatetheanalysisofunresolved, distantgalaxies.
P01ScaleSizeEvolutionofBrightestGalaxies
ClaireBurke (AstrophysicsResearchInstituteLJMU) with C. Collins, and J. Stott
Scalesizesofellipticalgalaxieshavebeenatopicofdiscussionrecentlyduetotheunexpectedresultthattheseobjectsevolvefromacompactstate.Wepresentourpreliminaryresultsofscalesizemeasurementsofbrightestclustergalaxies(BCGs)atz∼ 1, usingdeepimagingfromHST andSubaruMOIRCS of ∼ 10 BCGsinboththeopticalandnearinfra-red. WefindrobustBCG scalesizesof∼ 10kpc, andinferthatthisisevidenceformildsizeevolutionofthishomogeneouspopulationsincez∼ 1. Wediscussimplicationsofthisresult,inconcertwiththerecentresultofnomassevolutionofthesegalaxiesoverthesameperiod,forcosmologicalmodelsofthelatetimeevolutionofmassiveearlytypegalaxies.
Thecolours, AGN properties, environmentsandstarformationhistoriesofbulgedominatedpost-
mergersinthelocaluniverseAlfredoCarpineti (ImperialCollege)with
S. Kaviraj, and GalaxyZooteam
Galaxymergingisafundamentalaspectofthestandardhierarchicalgalaxyformationparadigm.InDargetal.(2010MNRAS.401.1043)wehavecreatedalarge, homogeneoussetofmergersthroughdirectvisualinspectionoftheentireSDSSusingtheGalaxyZooproject, apublicuserinterfaceontheworldwidewebforthemorphologicalclassificationofgalaxies. Atthetimeofwriting, over200,000volunteershavesubmittedover80millionclassificationsyieldingarobustcatalogueofaround3000mergerswhichhasbeenpresentedinDargetal. Weexploreasubsetofgalaxiesfromthiscataloguethatare'post-mergers', wheretheremnantappearstobeinthefinalstagesofrelaxation. Wefocusonpost-mergersthatshowevidenceforadominantbulge,makingthemplausibleprogenitorsofearly-typegalaxies. ForthissetofgalaxiesweexploretheirGALEX-SDSS UV/opticalcolours, AGN activity,localenvironmentsandstarformationhistories.64%ofourgalaxiesareeitherquiescentorshowLINER-likeemission, whiletherestareeitherstarforming(9%)orhaveSeyfertAGNs(25%). Wefindthattheplausiblemassratiosforthemergersthatcreatedthesesystemsarebetween1:1and1:10, withamedianvalueofaround1:3. Thespheroidalpostmergershavebluercoloursthanthegeneralellipticalgalaxypopulation, mostlikelyduetomerger-inducedstarformation.Comparisonwithstellarmodelssuggeststhatthestarformationactivityinmostofthesesystemspeakedlessthan1Gyrsago, suggestingthatsomeofstarformationrecentlydiscoveredinearly-typegalaxiesismerger-driven.
GalaxyClusteringUsingPhotometricRedshiftsLeonidasChristodoulou (UniversityofSussex)with
Jon Loveday, and GAMA Team
TheGAMA spectroscopicreleaseoffersauniqueopportunitytocalibratephotometricredshiftsfromSDSS downtor=19.4. TakingadvantageofthefactthatGAMA offersatrulyrepresentativesubsetofSDSS weconstructacatalogueof ∼ 5 million
Plenary–P01 43
objects, usinganartificialneuralnetwork(ANNz).Moreover, wecarryoutanextensiveerroranalysistocheckforpossiblebiasesinourredshiftsestimation. Wealsoshowindependentestimationsoftheunderlyingredshiftdistribution, usingaweightingmethod(Cunhaetal, 2009), whichrecoversmoreaccuratelytheredshiftdistribution.Thisallowsastorevealtheweaknessandthestrengthsofthetwomethods. Havingdonethat,wemeasurethetwopointangularcorrelationfunctioninluminositybinsandthenusingLimber'sapproximationwecalculatethespatialcorrelationfunction. Finallywecomparewiththeresultsintheliteraturefromspectroscopicsurveys.However, becauseoftheuseofphotometricredshiftsourworkextendstointrinsicallyfaintobjectswithmagnitudedowntoM=-14.
StudyinggalaxyevolutionwithFMOS (FibreMulti-ObjectSpectrograph)
EmmaCurtisLake (UniversityofOxford)withGavin Dalton, Thomas Mauch, Naruhisa Takato,
Naoyuki Tamura, Ian Smail, Philip Best,Jim Geach, David Sobral, and FMOS team
FMOS (FibreMulti-ObjectSpectrograph)isnowavailableontheSubaruTelescopeforobtainingnear-infraredspectraintheJ andH bands. With400targetfibres, withinawidefieldofview, thisinstrumentprovidesthemeanstoextendtheresultsfromlowredshiftspectroscopicsurveysusingthesamelinesasdetectedintheoptical. Inparticular, starformationcanbetracedbyH-αemissionbetween ∼ 0.5 < z < 1.7. I willgiveoverviewofFMOS andpresentinitialresults,includingspectroscopictargetingofHiZELS (High-Z EmissionLineSurvey)objects.
A newapproachtodisentanglingstarformationhistoriesfromsurveydata
IgnacioFerreras (UniversityCollegeLondon–MSSL)
Large, homogeneoussurveyssuchasSDSS orGAMA allowustoapplymultivariatetechniquesbasedatextractingdifferencesbetweenthestellarpopulationsofgalaxiesinamodel-independentway. InthistalkI willpresentrecentandongoingresearchfocusedonavolume-limitedsampleofearly-typegalaxiesfromSDSS.PrincipalComponentAnalysis(PCA) isusedtodefinetwoestimatorsofaverageageandrecentstarformationwhichisthenappliedtosubsamplesofclosepairsofearly-types(i.e. theprecursorsofdrymergers)ortosamplesclassifiedaccordingtothemassoftheparenthaloinordertoquantifytheeffectofenvironmentonthestarformationhistoryofgalaxies. Futuredirectionsforthepromisingfieldofmultivariateanalysisofphoto-spectroscopicdatawillbepresented.
A newsampleof"blazars"tostudytherelationshipbetweenradio-loudAGN andgalaxy
formationJenniferGupta (JodrellBankCentrefor
Astrophysics)with Ian Browne
Radio-loudactivegalacticnucleiarenowrecognisedtobevitalintheprocessofgalaxyformation, byprovidingfeedbackwhichregulatesthestar-formationprocess. Logicallyitfollowsthatinordertounderstandgalaxyformationandevolution, wemustunderstandAGN.However,thedetailsofhowAGN feedbackhappensisadifficultproblem; therearemanyunansweredquestions, suchaswhattriggerstheburstsofAGNactivity, howlongdotheburstsofactivitylastandhowdotheburstsevolve. Blazarsareasubsetof
radio-loudAGN whereoneoftheradiojetsisdirectedtowardstheobserveratasmallangletothelineofsight. Thereforeinblazarswegetthemostdirectviewoftherelativisticjetsthatmayultimatelyprovidethefeedback. Wehavedefinedanewsampleofnearbyblazar-likeobjects,attemptingtominimisetheselectioneffectsinordertounderstandthefundamentalandintrinsicpropertiesoftheseobjects. TheSurveyofExtragalacticNuclearSpectralEnergies(SENSE)samplecontains151compactradiocoreobjectswithin z < 0.2. HerewepresenttheSENSEsamplewithanemphasisonthewaysinwhichweareusingmultiwavelengthobservationsofthesampletoprobethephysicsofblazarsinthelow-redshiftUniverse.
GAMA photometryandtheCosmicSpectralEnergyDistribution
DavidHill (UniversityofStAndrews)withLee Kelvin, Simon Driver, Aaron Robotham, and
GAMA Team
Thecosmicspectralenergydistribution(CSED)describesthemeanradiationfieldwithinthesampledvolumeoftheUniverse. Itcangiveinsightintothestarformationhistory, andtheinitialmassfunction. Itsmeasurementrequiresaccuratephotometryfromanumberoffilters,whichhaspreviouslyledtodiscrepanciesbetweenopticalandNIR parameters. WeintroducetheGAMA photometricpipeline- amethodforgeneratingconsistentcoloursoverarangeofpassbands. WedescribethegenerationofGigapixelmosaicsandmatchedaperturecataloguesfromUKIDSS andSDSS data. Wequantifythesystematicoffsetsinbest-fittingluminosityfunctionparametersproducedbyusingdifferentaperturetypes, detectionthresholdsortotalmagnitudesystems. Finally, weintroduceaCSED,producedusingtheGAMA survey, andcompareittotheoreticalmodels.
Theradiospectralindexofsub-millimetregalaxies.
EdoIbar (UK AstronomyTechnologyCentre)withR.J. Ivison, P.N. Best, K. Coppin, A. Pope,
Ian Smail, and J.S. Dunlop
WehaveemployedtheGiantMetre-waveRadioTelescopeandtheVeryLargeArraytomaptheLockmanHole. At610and1400MHz, wereachnoiselevelsof15and6microJy/beam,respectively, withwell-matchedresolutions(∼ 5arcsec). Atthisdepth, weobtainedreliabledetectionsforabouthalfoftheknownsub-mmgalaxies(SMGs)inthefield(SCUBA,AzTEC andMAMBO).Forradio-identifiedSMGs, whicharetypicallyatz ∼ 2, wemeasureameanradiospectralindexof α(1400, 610) =-0.75±0.06(where Sν ∼ να)andstandarddeviationof0.29,betweenapproximaterest-framefrequenciesof1.8and4.2GHz. Theslopeoftheircontinuumemissionisindistinguishablefromthatoflocalstar-forminggalaxiesandsuggeststhatextendedopticallythinsynchrotronemissiondominatestheradiooutputofSMGs. CoolingeffectsbysynchrotronemissionandInverseComptonscatteringoffthecosmicmicrowavebackgrounddonotseemtoaffecttheirradiospectralenergydistributions. ForthoseSMGsjudgedbySpitzermid-infraredcoloursandspectroscopytohostobscuredactivegalacticnuclei(AGN),wefindacleardeviationfromtherestofthesample- theytypicallyhavesteeperradiospectralindices,α(1400, 610) . −1.0. Thesefindingssuggestthesemid-IR-/AGN-selectedSMGsmayhaveanintrinsicallydifferentinjectionmechanismfor
relativisticparticles, ortheymightresideindenserenvironments. Thisworkprovidesareliablespectraltemplatefortheestimationoffar-IR/radiophotometricredshifts, andwillenableaccuratestatisticalK-correctionsforthelargesamplesofSMGsexpectedwithSCUBA-2andHerschel.
Robustmethodstoprobesourceevolutioningalaxyredshiftsurveys
RussellJohnston (UniversityoftheWesternCape)
Oneofthemostfundamental, andstillrelevant,statisticalchallengesinmodernobservationalcosmologyisaccuratelydeterminingthegalaxyluminosityfunction. Determiningtheluminosityfunctionofgalaxiesremainsavitalandfundamentaltoolforassessingthestatisticalnatureofgalaxyformationandevolution. Pertinenttothisareaofstudyisaccuratelycharacterisingsourceevolutioningalaxyredshiftsurveys.
I willpresentarecentlydevelopedmethodthatrobustlyconstrainsluminosityevolutionarymodelsbyexploitingthepropertiesofthemagnitudecompletenesstestdevelopedbyRauzy(2001)andJohnston, Teodoro&Hendry(2007),combinedwithamaximumentropyapproach.Thisstatisticalapproachhasthepotentialadvantageovertraditionalapproachesbynotmakinganyassumptionoftheparametricformoftheunderlyingluminosityfunctionandisalsoindependentthespatialdistributionofgalaxies.
GAMA:SingleandMulti-ComponentGalaxyModelling
LeeKelvin (StAndrews)with Aaron Robotham,Simon Driver, Ewan Cameron, David Hill, and
GAMA Team
I presentresultsfromtheGAMA structuraldecompositionpipeline(GAMA-SIGMA;StructuralInvestigationofGalaxiesviaModelAnalysis)forallGAMA objectswithoptical-to-near-IR imagingfromtheSDSS &UKIDSS-LAS surveys. I showthatphotometricmodellingshorterthantheibandrestrictstherecoverabilityofgalacticproperties,anddiscusstheroleofdustinchangingourviewoftheUniverse. I alsodemonstratehowfullbulge-disk-bardecompositionisrequiredinordertogainfurtherinsightintotheformationandevolutionofgalaxies, anddiscussitsapplicationto ∼ 12,000nearbygalaxiesintheforthcominghigh-resolution/deepVST &VISTA imagingoftheGAMA fields.
TheALFALFA HI AbsorptionSurveyErinMacdonald (UniversityofGlasgow)with
Jeremy Darling, and ALFALFA Team
Wepresenttheresultsofawide-areapilotsurveytosearchforcoldNeutralHydrogen(HI) 21cmabsorptionutilizingtheAreciboLegacyFastAreciboL-BandFeedArray(ALFALFA) Survey. Thissurveyisthefirsttoconductawide-area(517.0deg2)''blind''searchforHI absorptioninthelocaluniverse. Thesurveyspans 10.9h < α < 14.95h
and +7.7◦ < δ < 6.3◦ centredontheVirgoCluster. ThefullALFALFA surveyisanHI emissionsurveythatcovers−650 ∼ km ∼ s−1 < cz < 17, 500 ∼ kms−1
(11% ofthisspanislosttoradiofrequencyinterferenceandGalacticHI emission)resultingina ∆z=0.054alongeachlineofsight. Whencompleted, theALFALFA surveywillspan7000deg2. OursurveyissensitivetoHI absorptionlinestowardsradiosourcesstrongerthan8.4mJy.Thisincludes8983sourcesforatotalsearchpathof ∆z = 485.1. Thereare243sourcestoward
44 P01
whichalldampedLy-α systems(N(HI) > 2 × 1020 cm−2)couldbedetected,and3282sourcestowardwhichN(HI) > 2 × 1021 cm−2 columnscouldbedetected. WedetectonepreviouslyknownHIabsorptionlineinUGC 6081, confirmingourmethodisfeasible, butmakenonewdetections.Usingthesedata, wecalculateanupperlimittotheHI columndensitydistributionfunctionanditsmoments. Thispilotsurveydemonstratesthevalueandfeasibilityoflarge-arearadioabsorptionlinesearchesthatarenotyetpossiblewithopticaltelescopesandprovidesabaselineforfutureHI 21cmabsorptionlinesurveysplannedfornewradiofacilities, suchasSKAMP,ASKAP,MEERKAT andtheATA.
ModellingtheUV/opticalFIR/submmemissionfromSpiralGalaxies
CristinaC.Popescu (JeremiahHorrocksInstitute,UCLan)with RichardJ. Tuffs
WepresentacomprehensivelibraryofspectralenergydistributionsofspiralgalaxiesintheMIR-submmrangecalculatedasafunctionofaminimalsetofphysicalparametersusinganupdatedandenhancedversionofthemodelofPopescuetal. (2000). Wedescribehowthissetofdust/PAH re-emissionSEDscanbeself-consistentlycombinedwiththeexistinglibraryofUV/opticaldustattenuationscalculatedusingthesamemodel(Tuffsetal. 2004)toinvertanobservedsetofbroad-bandphotometryofagalaxyspanningtheUV/optical- FIR/submmrangetoderivetheintrinsic(i.e. aswouldbeobservedintheabsenceofdust)UV/opticalemissionofthegalaxy. UsingrealandsimulateddataweillustratetheapplicationoftheSEDmodellingtechniquetothederivationofstarformationratesandstarformationhistoriesofopticallyselectedspiralgalaxiesinthelocalUniverseobservedbyGAMA andHerschel.Specifically, wequantifyhowtheamplitudeandwavelengthdependenceoftheUV/opticalattenuationisrelatedtotheamplitudeandcolouroftheFIR/submmcontinuumemissionmeasuredusingthePACS andSPIRE instruments, anddescribehowtoutilisemorphologicalinformationfromhigherresolutionopticalobservationsofGAMA galaxies(suchaslinearsizesofdisksandthebulge-diskdecompositions)intheinterpretationofthepanchromaticobservations.
RedandBlueSatelliteGalaxiesintheGalaxyandMassAssemblySurvey
MatthewPrescott (LJMU AstrophysicsResearchInstitute)with IvanK. Baldry, PhilA. James, and
GAMA Team
Theroleofblue-sequencesatellitegalaxiesinthefuellingofdiskgalaxies. A long-standingproblemfordiskgalaxiesistheoriginofthecontinuinggassupplyrequiredtoexplaintheirstarformationandchemicalabundanceproperties. Onepossiblesourceisfromgas-richsatellites, eitherthroughminormergers('cannibalism')orfromthegascomponentonlyofthedwarfbeingtransferredtothediskgalaxy, withthegasremovaloccurringeitherthroughtidesorthroughsupernova-drivenwinds. Aninitialsearchforgas-richcompanionsoffielddiskgalaxiesusingwide-fieldH αimagingshowsthatMagellanicCloud-likesatellitesaresurprisinglyrare. Thescarcityofgas-richcompanionscouldbeindicativeoftheefficiencywithwhichtheyhavebeengas-strippedandtransformedintored-sequence, passivedwarfs. InthistalkI willpresentthepreliminaryresultsofastudyonthered-to-blueratioofdwarfgalaxies
aroundisolatedfielddiskgalaxiesselectedfromtheGAMA survey, andthevariationinthisratioasafunctionofprojectedseparation.
AbundancegradientsinsimulatedgalaxydiscsAwatRahimi (UniversityCollegeLondon–MSSL)
with Daisuke Kawata, ChrisB. Brook,BradK. Gibson, and Carlos Allende-Prieto
TBC
GalaxyAndMassAssembly(GAMA):Thenextgenerationsurveyofsurveys.
AaronRobotham (StAndrews)with GAMA Team
TheGAMA surveyisthelatestgenerationphotometricandredshiftsurvey. ItwillcoverthefullSED ofgalaxies, fromtheFUV totheradio, andiscomplementedby130,000redshiftsobtainedfromtheAAT overa3yearperiod(finishingMay2010). GAMA willprobestructureoverthescalesof1kpcto1Mpc, helpingustounderstandgalaxyformation, theenergyoutputoftheUniverse, andtheroleofgroupsandclustersingalaxyevolution.
Modellingradiationfieldsingalaxiesusinganewradiationtransfercode
DmitrijSemionov (JeremiahHorrocksInstitute,UCLan)
Wedescribeanewraytracingradiationtransfer(RTR) codebeingdevelopedatUCLan, optimisedforcalculatingthedistributionofradiationfieldsindustygalaxies. PrimaryapplicationswillbetomodelimagesandintegratedSEDsindirectanddustre-radiatedlightofsyntheticgalaxiescalculatedselfconsistentlywithCDM cosmology.
NGC 2976&NGC 3351: 12CO(3-2)ObservationsanditsCorrelationwithPAH 8um
BoonKokTan (UniversityofOxford)withJamie Leech, Dimitra Rigopoulou, and NGLS
teammembers
Wepresent12CO(3 − 2) mapsofNGC 2976andNGC 3351obtainedusingtheJamesClerkMaxwellTelescope. BothgalaxiesarepartoftheNearbyGalaxyLegacySurvey(NGLS).Wecombinethesedatawiththe12CO(3 − 2) mapsfromNobeyamaRadioObservatoryandBerkeleyIllinoisMarylandAssociationinterferometertoderiveCO line-ratiomap. Thevalueof12CO(3 − 2) to12CO(1 − 0) lineratioweobtainedwaswithin0.2--0.6range. Usingthisratio, wederivedthetotalmoleculargasmassof3×107 solarmassforNGC 2976and7.55x108
solarmassforNGC 3351. Wepresentspectralmapsanddiscussthevelocityfieldandthevelocitydispersionofthetwogalaxies. WefindthatthesevelocitycomponentsareverysimilartothedatafromtheVLA surveyofHI emission.Using8umSpitzerdata, weinvestigatedthecorrelationofthe12CO(3 − 2) intensitywiththePAH 8micronsurfacebrightness. Westudytheradialdistributionofthesestarformationtracersinthetwogalaxiesandsuggestthatthecorrelationisgoodathighsurfacebrightnessregion. Weextendthisstudytoincludethetotalsurfacebrightnessofthe12CO(3 − 2) andthePAH 8 µmemissionof17galaxieswithintheNGLS samples. Wefindthatthecorrelationisverygoodatlargespatialscale, asbothphysicalparameterstraceactivestarformation.
P02Anultravioletstudyofthetheweakwind
probleminO starsMatthewAustin (UCL) with Raman Prinja
Learningthefinerdetailsaboutmass-lossfromstarsofearlyspectraltypeisimperative. Theimpactofthisenergeticphenomenonisgreat,acrossalargesliceofastrophysics. Recently,determiningtruemass-lossratesinO starshasbeenhamperedbydiscordantspectraldiagnostics.WedescribeanefforttocomputetherunofionfractionwitheffectivestellartemperatureforthewholeO starrange, forC,N,O,P,S andSi. WegivedetailsconcerningtheprojectundertakentofitC IV resonancelineprofilesinlateO dwarfsandhighlightthemagnitudeofthecurrentproblem.
ProbingSitesofMassiveStarFormation: TheMethanolMultiBeamSurvey
AdamAvison (JodrellBankCentreforAstrophysics)with Gary Fuller, James Caswell,
James Green, and MMB Collaboration
TheMethanolMultibeamsurveyisagalacticplanesurveyforClassII methanolmasersat6.7GHz. TheseuniquetracersofmassivestarformationhavebeenobservedusingapurposebuiltsevenbeamreceiverontheParkesradiotelescope, withhighresolutioncounterpartobservationstakenattheAustraliaTelescopeCompactArraytoachievehighaccuracypositions.
ThesouthernhemisphereobservationsisnowcompleteandthefirstcatalogueofMMB resultscoveringthegalacticcenterregion(345o-> 0o-> 6o)hasrecentlybeenreleased(Caswell2009).ThisalongwithacompletesurveyoftheLargeMagellanicCloud(Green2008)highlighttheinterestingresultsthesurveyisalreadyyielding.Workiscurrentlyongoingtocomparethelocationsofmassivestarformationsignpostedbythe6.7GHzmaserswithotherdataofthegalacticplanei.e. infraredsurveys(MIPS,GLIMPSE),excitedOH masersandsoontobetakenmolecularlineobservations. InthistalkI willaddressthelatestresultsoftheMMB surveyanditsfutureprospects.
SurveyoftypeIb/csupernovaprogenitorsinnearbystar-forminggalaxies.
JoanneBibby (UniversityofSheffield)withPaul Crowther
Pre-supernovabroad-bandimagingofgalaxieshasrevealedtheredsupergiant(RSG) progenitorofTypeII SNe. However, whilstWolf-Rayet(WR)starsarebelievedtobetheprogenitorofTypeIb/cSNeadirectobservationallinkisyettobeestablished. Bysurveying ∼ 10 nearbystar-formingspiralgalaxieswithVLT andGeminiweaimtoproduceacatalogueofWR starswhichcanbereferredtowhenaTypeIb/cSNeoccurs.
I summarizethenarrow-bandimagingtechniqueusedtoidentifyWR stars, alongwithMulti-ObjectSpectroscopyMOS) confirmation. I considerthelimitationsofground-basedimagingwithcomparisontoHST archivaldata. BydegradingthespatialresolutionofarepresentativesampleofLMC Wolf-Rayetstars, tothatofatypicalgalaxyinoursample, weaddressthequestionofcompleteness. WeaskwouldtheWR emissionstillbeobservedorwoulditbedilutedtothepointitwasnolongerdetectable?
P01–P02 45
Finally, I willdiscusscompletedsurveysinoursampleandhowtheyarebeingusedtoinvestigatewhetherthespatiallocationofdifferentWRsubtypescorrelateswiththelightdistributionofthehostgalaxy. Moreover, wecancomparethespatiallocationoftheWR starswithbothTypeIb/cSNeandGRBs.
A wide-field, high-resolutionviewofNGC2264JaneBuckle (UniversityofCambridge)with
J.S. Richer
Understandingthephysicsofwhereandhowstarsformisafundamentalastrophysicalquestion. Theprocessesassociatedwithstarformationareimportant: onlargescales, inthestructureandevolutionofgalaxies, tosmallscales, intheformationofplanets. Starformationoccursindensecoresinmolecularclouds, andmassivestarsforminclustersofmixedmassstars. Studiesofyoungclustersarethereforeessentialforunderstandingmassivestarformation.
NGC2264isanattractiveregiontostudy; at800pcitisoneofthenearestregionsofclusteredstarformation, andcontainstwoyoungprotoclusters.Oneoftheseisthoughttobeformingamassivestarof10-20solarmassesinthecentreofthecluster, fromthegravitationalmergerofintermediate-masscores.
Wepresentwide-field, highresolution2-D and3-D imagingofthisstarformingregioncovering1squaredegree, inUKIRT WFCAM H2narrow-band1-0S(1) lineemissionandJCMT HARP J=3-2CO emission. ThroughCO spectralimaging, wecanprovideacompletecensusofprotostellaroutflowactivityintheregion, investigatingthedynamicimpactoftheoutflowsonthenatalcloud. H2emissionhighlightstheyoungestflows,fromemissionarisingingasshockedbytheimpactofoutflows. Weusethisimagingdatatomeasuretheextentoftheveryyoungestflowsinthestarformingclusters.
Multiplegenerationsofmassivestarformationinclustercomplexes
SimonClark (OpenUniversity)with M. Messineo,H. Parsons, B. Davies, and M. Thompson
Theprocessesgoverningtheformationofmassivestarsarepoorlyunderstood, primarilyduetoobservationaldifficultiesresultingfromtheirrarityandhighextinction. Neverthelessitisthoughtthattheypredominantlyforminstaraggregates, whichinturnarefoundwithinlargerclustercomplexesassociatedwiththenatalGMC.Wepresenttheintialresultsofanextensivemultiwavelengthobservingcampaignaimedatconstrainingthestarformationhistoriesofsuchcomplexesandthepropertiesofthecoldprotostellarcoresandthe(proto-)stars/clustersfoundwithin, inordertoprovideconstraintsonthephysicsyeildingthem.
TheRMS Survey: NearInfra-RedSpectroscopyofMassiveYoungStellarObjectsInTheNorthern
HemisphereHeatherCooper (UniversityofLeeds)with RMS
Team
TheRMS surveyisthelargestcomprehensive,galaxy-widesurveyofmassiveyoungstellarobjects(MYSOs)todate. Colourcutsdefinedusing2MASS andMSX datawereusedtoselectmid-IR brightpointsourcesfromtheMSX satellitesurvey, producingaround2000candidateMYSOs.A seriesofmultiwavelengthfollow-upobservationshavebeendonetoclassifytheseobjectsandcharacterisetheMYSOsandH II regions. Asthe
finalstageofthisprocess, near-IR spectrahavebeenusedtodistinguishtheremainingH IIregions, oldstarsandothersourcesfromthegenuineMYSOs. Withthesenear-IR follow-upobservationscompleteinthenorthernhemisphere,andnearingcompletioninthesouthernhemisphere, thepreliminaryresultsandplansforexploitationofthenear-IR datawillbediscussed.
A MassiveStarisBorn: thecircumstellardisk,envelope, andbi-polaroutflowofW33A
BenDavies (RochesterInstituteofTechnology, NY)with S.L. Lumsden, M.G. Hoare, R.D. Oudmaijer,
and W.-J.de Wit
TheYoungStellarObject(YSO) W33A isoneofthebestknownexamplesofamassivestarstillintheprocessofforming. Wepresentnear-infraredhighspatialresolutionintegral-fieldspectroscopyofW33A,andfindevidencefor(a)arotationally-flattenedouterenvelopeataradiusofseveralthousandAU,(b)ahotcircumstellardiskataradiusof1-3AU,and(c)afastbi-polarionisedoutflowonsub-milliarcsecondscales, whichisalignedwiththeobject'slarger-scaleoutflow.Fromthekinematicsofthematerialintheinnernebula, wefindthatthecircumstellardiskorbitsacentralmassof > 10M⊙, whiletheouterenvelopeenclosesamassof ∼ 15M⊙. Theseresultsthereforeprovidestrongsupportingevidenceforthehypothesisthattheformationmechanismforhigh-massstarsisqualitativelysimilartothatoflow-massstars.
TheVLT-FLAMES TarantulaSurveyChristopherEvans (UK ATC)
30DoradusintheLargeMagellanicCloudisthelargestHII regionintheLocalGroup, providinganideallaboratoryforstudiesofstellarandclusterevolution. I willgiveanoverviewoftheVLT-FLAMES TarantulaSurvey, anESO LargeProgrammewhichhasobtainedmulti-epochopticalspectroscopyofover800OB-typestarsin30Dortoaddressfundamentalquestionsofmassivestarevolution, suchasmultiplicity, mass-loss, chemicalenrichmentviarotation, andclusterdynamics.
TypeIbcsupernovaeindisturbedgalaxies:evidenceforatop-heavyIMF
StaceyHabergham (AstrophysicsResearchInstitute)with J.P. Anderson, and P.A. James
Wecomparetheradiallocationsof169core-collapsesupernovaetotheR-bandandH αlightdistributionsoftheirhostgalaxies. Whenthegalaxiesaresplitinto'disturbed'and'undisturbed'categories, astrikingdifferenceemerges. Thedisturbedgalaxieshaveacentralexcessofcore-collapsesupernovae, andthisexcessisalmostcompletelydominatedbysupernovaeoftypesIb,IcandIb/c, whereastypeII supernovaedominateinallotherenvironments. Thedifferencecannoteasilybeexplainedbymetallicityorextinctioneffects, andthusweproposethatthisisdirectevidenceforastellarinitialmassfunctionthatisstronglyweightedtowardshighmassstars,specificallyinthecentralregionsofdisturbedgalaxies.
High-MassX-rayBinariesintheNIR:Orbitalsolutionsoftwohighlyobscuredsystems.
AndrewMason (OpenUniversity)withA.J. Norton, J.S. Clark, I. Negueruela, and P. Roche
I presentNIR spectroscopyobtainedusingtheVLTandISAAC oftwoeclipsingX-raypulsars, OAO
1657-415andEXO 1722-363. Bothofthehigh-massdonorstarsinthesesystemshaveonlyrecentlybeendiscovered, duetotheirhighlevelsofextinction. I willinitiallydiscussourworkinspectrallyclassifyingthetwodonorstars. ThedonorintheEXO 1722systemwasfoundtobeatypicalofthisclassofHMXB.ThedonorwithinOAO 1657wasfoundtobeamoreevolvedOfpe/WN9star. TheseresultsthrowlightontheunusualpositionofOAO 1657-415intheCorbetdiagram. Wehaveconstructedradialvelocitycurvesforbothofthesesystems, andI willpresentorbitalsolutionsandthefirstNS massdeterminationsmadeutilisingNIR spectroscopyforeachsystem.
TheevolutionofthepeculiarvariableV838Monocerotis2002-2009
MarkRushton (JeremiahHorrocksInstitute,UCLan)with M.T. Rushton, T.R. Geballe, A. Evans,
and S.P.S. Eyres
ThepeculiarvariableV838Monocerotiswasdiscoveredineruptionin2002andtransformedfromaK-typestarintothecoolestknownsupergiant. Sincethen, itsnear-infraredspectrumhasbeendominatedbystrongmolecularbands,andisreminiscentofthatofanL-typebrowndwarf. However, V838Moncontinuestoevolverapidly. Wepresentnear-infraredspectroscopyoftheobjectobtainedonmultipleoccasionsbetween2002and2009, showingthechangesthathaveoccuredinthatperiod. ThecauseoftheoutburstofV838Monisuncertain, butthediscoveriesofaB-typecompanionandanearbyclusterofstarsshowstheobjectistooyoungforanova, oraverylatethermalpulse. Theleadingexplanationisastellarmerger.
P03DoBBF eventscontributetoinnermagnetospheredipolarisation? A threeyearstatisticalstudyusingconcurrentClusterandDoubleStarobservationRogerDuthie (UniversityCollegeLondon–MSSL)with Andrew Fazakerley, Iannis Dandouras, and
Elizabeth Lucek
TheobserveddynamicalphenomenonofflowinEarth’smagnetotailwhichisintermittent, high-speed&non-fieldalignedistermed“burstybulkflow”(BBF).Dipolarisationofthemagneticfieldwithinthenight-sidemagnetosphereofEarthmaybecausallylinkedtoBBFs. BothphenomenaareattributedtotheEarth'ssubstormcycle.Competingmodelsattemptingtoexplainsubstormprocesses, andthecausallinkbetweenBBF anddipolarisation, havestilltobeconclusivelyverifiedorfalsified. Thesearechieflythecurrentdisruption(Lui1991)&near-Earthneutralline(Bakeretal1996)models. A statisticalstudyhaspreviouslybeenperformed(Takadaetal2006)throughconcurrentobservationsbyCluster4(“Tango”)&DoubleStarTanCe1, makinguseofmagnetotaildatafromoneyear. ItwasfoundfromthisthatathirdoftheBBF eventsdetectedbyCl4hadwiththemanassociateddetectionofadipolarisationeventbyTC1. Thestatisticalresultssuggestedthatthespacecraftseparationwasgenerallyshorter, andthemagneticfieldatTC1typicallyhadasmallerpolarcomponent, whenassociationbetweendetectionswasfound.Additionally, near-geosynchronousregion(R ∼ 6.6RE )dipolarisationstendednottohaveanassociationwithBBF eventdetections. The
46 P02–P03
presentstudyextendsthetimeintervaltothreeyears. ThefindingsfromtheobservationofBBF &fielddipolarisationscantherebybefortifiedandimproved. Issuesraisedbythepreviousstudycanbealsobemorefullyaddressed.
Lui(1991)A synthesisofmagnetospherissubstormmodels, J.Geophys. Res., 96, 11,389-11,401Bakeretal(1996)Neutrallinemodelofsubstorms;Pastresultsandpresentview, J.Geophys. Res.,101, 4967-4989Takadaetal(2006)DoBBFscontributetoinnermagnetospheredipolarizations:ConcurrentClusterandDoubleStareobservations,Geophys. Res. Lett., 33, L21109
AveragepropertiesofthemagneticreconnectioniondiffusionregionintheEarth’smagnetotail:
2001–2005Clusterobservationsandcomparisonwithsimulations
JonathanEastwood (ImperialCollegeLondon)with T.D. Phan, M Oieroset, and M.A. Shay
CollisionlessmagneticreconnectionplaysakeyroleinthedynamicsoftheEarth’smagnetosphere.Ofparticularimportanceisthediffusionregion,sincethisiswherethemagneticfieldultimatelyreconnects. Althoughconsiderableprogresshasbeenmadeinrecentyears, manyquestionsremain, inpartbecauseitisdifficulttomakein-situobservationsofthisregion, andsorelativelyfewindividualeventshavebeenreportedintheliterature.
Toaddressthisproblem, theClustermagnetotaildatasetfrom2001- 2005(constituting175magnetotailpasses)hasbeencomprehensivelysurveyedforencounterswithreconnectionsitesintheplasmasheetbysearchingforcorrelatedreversalsinthenormalmagneticfieldandtailward/earthwardplasmaflow. Thissurveyresultedin33events. Oftheseevents, 23(70%)wereinqualitativeagreementwiththeexpectedpatternofHallfields, indicatingadiffusionregionencounter. Withinthesetofdiffusionregionencounterscorrespondingtoanti-parallelreconnection, theabsolutesizeofboththeHallelectricandmagneticfieldwerebothfoundtovaryfromeventtoevent. However, withappropriatenormalizationtotheobservedboundaryconditions, consistentmagnitudesofboththeaveragepeakHallmagneticandtheaveragepeakHallelectricfieldarefound. Tobetterunderstandthisexperimentaldata, largeparticle-in-cellsimulationswereperformed,normalizedinthesamewayasthedata. Acomparisonoftheobserveddataandthepredictionsofsimulationswillbeshown.
TheseresultshelptoestablishtheoccurrencerateofdiffusionregionsrelativetomacroscopicsignaturesandtheaveragepropertiesofthediffusionregionintheEarth'smagnetotail. Wealsodiscussthemostusefulsignaturesforestablishingexperimentallythein-situmeasurementofdiffusionregions.
10YearsofCluster: HighlightsofMulti-pointMeasurementsinSpacePlasmas
C.PhilippeEscoubet (ESA/ESTEC) withM.G.G.T. Taylor, A. Masson, H. Laakso, and
M. Goldstein
Afteralmost10yearsofoperations, theClustermissionisfulfillingwithgreatsuccessitsscientificobjectives. ThemaingoaloftheClustermission,madeoffouridenticalspacecraft, istostudyinthreedimensionsthesmallandmedium-scaleplasmastructuresinthekeyplasmaregionsoftheEarth’senvironment: solarwindandbowshock,
magnetopause, polarcusps, magnetotail, andauroralzone.
Duringthecourseofthemission, therelativedistancebetweenthefourspacecrafthasbeenvariedfrom100to10,000kmtostudythescientificregionsofinterestatdifferentscales.Sincesummer2005, newmulti-scaleconstellationshavebeenimplemented, wherethreespacecraft(C1, C2, C3)areseparatedby10000km, withthefourthone(C4)atavariabledistancefrom40to10000kmfromC3.
Wewillhighlightsomeofthemainresultsfromthelast10years: evolutionofblackauroras, firstdirectmeasurementsofelectriccurrents,observationofthelargestreconnectioneventof2.5millionkminlength, observationsofgiganticsurfacewaves, firstevidenceofreconnectioninturbulentplasmaandusageofinterferometrytolocaliseelectromagneticemissions. ThepresentationwillalsocoverClusterdataaccessibility, throughtheClusterScienceDataSystem(CSDS) andtheClusterActiveArchive(CAA) whichwasimplementedtoprovideapermanentarchiveofhighresolutionClusterdatafromallinstruments.
Multi-spacecraftobservationsofauroralelectronaccelerationbyCluster
ColinForsyth (UniversityCollegeLondon–MSSL)with A.N. Fazakerley, A.P. Walsh, K. Garza,
C.J. Owen, I. Dandouras, K-H. Fornacon, andE. Lucek
DuringrecentyearstheorbitoftheClusterspacecrafthasevolvedsuchthatthespacecraftpassthroughtheauroralaccelerationregionclosetoperigeeduringthedaysideseason. Thispresentstheopportunitytomakemulti-spacecraftmeasurementsofthisregionforthefirsttime.
WepresentacasestudyofanupwardauroralcurrentregionobservedbyClusterinDecember2009. Duringthisevent, Cluster1andCluster3wereapproximatelylocatedonthesamemagneticfield-linebutseparatedby1000km. Weshowthattheelectronpopulationwasacceleratedalongthefield-linebetweenCluster1and3. Magneticfieldobservationsconfirmthepresenceofanupwardcurrentsystem. Basedontheseobservationsweestimatethesizeofthelengthoftheaccelerationregion.
ExtendingClusterJSOC scienceoperationsoverthepasttenyears
MikeHapgood (STFC RutherfordAppletonLaboratory)with M.G. Hutchinson,
M.A. Hapgood, T.G. Dimbylow, P.A. Chaizy, andA. McDermott
JSOC hassuccessfullyco-ordinatedthescienceoperationsofESA'scornerstoneClustermissionfortenyears. Theoriginalmissiondurationwastwoyearsandextendingthescienceoperationsbeyondthisperiodhasbeenatechnicalandmanagementchallenge, especiallyasthespacecraftandinstrumentsage, andstaffleaveandarereplaced. Furthermore, thesciencegoalsofClusterhaveevolvedinresponsetoscientificadvancesandtonewscientificopportunities(providedbyorbitalevolutionandbycollaborationwithnewexperimentsinspaceandontheground). Meetingthesechallengeshasbroughtconsiderableimprovementsandpositiveinsightsinco-ordinatingscienceoperations,includingthestructuredspreadingofexpertisewithintheteamtominimiseriskandincreaseflexibilityaswellasbuilding-inincreased
automationandimprovedsafetycheckingviarule-basedplanningtechniques. Importantly, expertisehasbeengainedinthetheoreticalandpracticaldevelopmentanduseofgenericplanningconceptsandsystemsaimingatimprovingthescientificreturnandthecostefficiencyofspacesciencemissions, includingmulti-pointmissions.
UsingCluster’sobservationsofthesolarwindtoinvestigatecollisionlessplasmaturbulence--
currentresultsandoutlookforthefutureKhuromKiyani (UniversityofWarwick)with
A. Turner, S.C. Chapman, B. Hnat,Yu. V. Khotyainstev, and F. Sahraoui
In-situobservationsofmagneticfluctuationsinthesolarwindshowan‘inertialrange’ofMHDturbulence, andathigherfrequencies, across-overtoscaleswherekineticeffectsbecomeimportant.Thiscrossoverisseeninthepowerspectraldensity(PSD) asasecondbroad-bandpowerlawregionextendingfromthetypicalionLarmorscaleofthesystemtoelectrongyroscales. Theoreticalstudiesofplasmaturbulencepredictthenatureofthescalinginthisregioncentredaroundpredictionsofthespectralslopeandassociatedscalingexponents.
Wepresentresultsfromhigh-frequencymagneticfielddatafromClusterinintervalswherethespacecraftwereinquasi-stationaryambientsolarwindandtheinstrumentswereoperatinginburstmode. Themagneticfielddataarefromthefluxgateandsearch-coilmagnetometersfromtheClusterFGM experiment(∼ 67Hz), andtheSTAFFexperiment(∼ 450 Hz). Thesedatasetsprovideobservationsofthissecondscalingrangeovertwodecadesinfrequency. Thishighcadenceallowsaprecisedeterminationofthestatisticsatthesesmallscales.
WeperformarobustmultiscalestatisticalanalysisfocusingonthePSD,PDFsoffieldfluctuations,higher-orderstatisticstoquantifythescalingoffluctuations; aswellasdescribingthedegreeofanisotropyinthefluctuationsparallelandperpendiculartotheaveragelocalmagneticfield.
Thestudyofsolarwindturbulencepresentssomechallengestosomerecentandfuturemissions.CurrentlyClusterstillpossessessomeofthebestaccessibleobservationsofkineticscaleelectromagneticwaveforms–evenafter10years.Toanswertheopenquestionofhowcollisionlessturbulenceisdissipatedintoheatingthesolarwind, weneedtopushfurtherthetelemetryandsensitivityofmeasurementsfromfuturemissions.WeconcludebydiscussingthesourcesoferrorfrominstrumentnoiseandouroutlookonhowClustercaninformfuturemissions.
Here, thereandeverywhere: gettingafeelforboundarylayerevolutionusingmultipoint
measurementsMattTaylor (EuropeanSpaceAgency)with I.J. Rae,
C. Watt, K. Nykyri, B. Lavraud, A.N. Fazakerley,M.W. Dunlop, A. Borg, H. Laakso, C.P. Escoubet,A. Masson, M.N. Nishino, M. Lester, S.E. Milan,J.A. Davies, L. Kistler, C. Mouikis, M. Volwerk,
A. Grocott, C. Forsyth, A.P. Walsh, A. Lui, C. Shen,Z. Pu, and J. Shi
Onthe11thJuly2006, duringaperiodofnorthwardIMF,theGeotail, DoubleStar1andClusterspacecraftallcrossedthemagnetopauseregionwithin2hours(UT) ofoneanotherwhileseparatedbymanyhoursinlocaltime. Duringthistimelarge-scaleoscillationswereobservedinbothgroundbasedandspacecraftdata. Weutilize
P03 47
thesenumerousmeasurementstoexaminetheextentandevolutionoffluctuationsinandaroundthemagnetopauseboundarylayer. ThisworkisbeingcarriedoutaspartofanInternationalSpaceScienceInstitute(ISSI) workinggroupon‘ComparativeCluster- DoubleStarmeasurementsoftheMagnetotail’.
TheMagnetotailPlasmaSheetRevisited: ClusterPEACE Statistics
AndrewWalsh (UniversityCollegeLondon–MSSL) with A.N. Fazakerley, C. Forsyth, and
C.J. Owen
WiththeClusterActiveArchivenowcontainingalargevarietyofhigh-quality, validateddataproducts, thereisanopportunitytocarryoutlarge, multi-instrumentstatisticalstudiesusingClustermeasurements. Wepresentfirstresultsfromonesuchstudy: asurveyofelectronpitchangledistributionsmeasuredbyClusterPEACEduringthe2002tailseason(July- October). Intotal ∼ 850,000distributionshavebeenexaminedintermsofmagneticfieldstrength, auroralindicesandotherparameters. Wefindthatthemagnetotailplasmasheetisonlyroutinelyisotropicwhen|B| < 3nT,i.e. closetotheneutralsheet. Outsidethisregionalow-energyfield-alignedpopulation, presumablythatidentifiedbyAsnesetal. (2008), waspresentatalllevelsof|B|.Significantelectronfluxeswerefoundtoextendtohigher|B|athigherAL/AE andexhibitedenergy-dispersedbehaviouratthehigh|B|edge. TheslopeofthisdispersionalsochangedwithAL/AE.
P04X-rayBrightPointTopologyStudywithHinode
andSTEREOCarolineAlexander (JeremiahHorrocksInstitute,
UCLan)with R.W. Walsh, M. Marsh,R.C. Maclean, and G. DelZanna
Wepresentacasestudyofamediumsized(∼ 15")X-raybrightpointobservedwithHinodeandSTEREO.Wehavestudiedtheevolutionandtopologythroughoutitslifetimeandpresentresultsonphysicalcharacteristicsaswellasstructure.Thetopologyhasbeenstudiedusingavarietyofmethods. PotentialfieldextrapolationshavebeencarriedoutandcomparedwithX-rayimagesfromXRT.Edge-detectionimageprocessinghasthenbeenusedonXRT imagestoseeifthisclarifiesanyloopstructurepresent. STEREO datahasalsobeenusedtoexplorethe3D topologyandinvestigatewhatline-of-sighteffectshaveonpreviousresults.
PlasmaMotionsandMagneticReconnectionHeatinginthe2007, May19Flare
LenCulhane (UniversityCollegeLondon–MSSL)with H. Hara, T. Watanabe, L.K. Harra, and
P. Young
WereportobservationstakenwiththeHinodeEISspectrometerofaloop-tophotsource, anearbyfastjetandaninflowtothehotsourceregionduringtheimpulsivephaseofalongdurationGOES ClassB9.5flareon2007, May19. TheeventwasalsoobservedwiththeHinodeSolarOpticalandX-rayTelescopes(SOT,XRT),RHESSIandTRACE.Intheimpulsivephase, EIS wasscanningaregionaboveFeXVII (192Å) andCaXVIII (255Å) emittingloopsatT ∼ 5 MK withasmallcusp-shapedapex. Theregionabovetheloopshas12MK hotplasmacomponentsthat
wereobservedinFeXXIII (263Å) andFeXXIV(192Å,255Å) emissionandintheRHESSI 4–6keV band. Atthepeakoftheimpulsivephase, thishotthermalsourceshowedexcesslinebroadingindicatingnon-thermalvelocitiesof ∼ 100 km/sandaweakredshiftof ∼ 30 km/s. A blue-shiftedjetwithaDopplervelocityof200km/sisalsoobserved. ThereisalsoacoronalstructureseeninFeXII 195Å emissionwithmaterialflowingintothehotsourceregionat ∼ 20 km/s. Twonon-thermalhardX-raysourcesareseenwithRHESSIinthe15–40keV band. Oneincludesbothoftheflaringloopfootpointswhiletheotherisfoundabovethelooptop. Alloftheseobservationsareconsistentwiththelocationofamgnetticreconnectionsitenearthehotsourceregionandthecusp.
Hinode/EIS observationsofactiveregionloopsGiulioDelZanna (UniversityofCambridge)
NewmeasurementsofelectrontemperaturesanddensitiesinactiveregionloopsobtainedwiththeHinode/EIS spectrometerarepresented. Theyareobtaineddirectlyfromlineratiosandnewatomicdata. ThesemeasurementsarecomplementarytothosepreviouslyobtainedonDopplermotions,and, oncerefined, willallowdetailedcomparisonswithresultsfromtime-dependentmodelling. Newobservationalandtheoreticalchallengesarebrieflydiscussed.
ObservationsofflareribbondensitiesusingHinode/EIS
DavidGraham (GlasgowUniversity)withLyndsay Fletcher
WepresentnewhighcadencemeasurementsofplasmadensityandbulkflowvelocitiesinasolarflareusingobservationsfromHinode/EIS andTRACE.Wehavefoundapparentdensityenhancementsinchromosphericflareribbonsandfootpoints, derivedusinglineratiosinFeXII,FeXIII andFeXIV.Bycombiningthesewithco-spatialvelocitymeasurements, weseesignsofcompressionandexpansionoftransitionregionandchromosphericplasma, inresponsetotheflareenergyrelease. Amongtheseobservationsaredensityenhancementslastingwellintothedecayphaseoftheflare, andsignsofasymmetricalblueandredshiftsacrossfootpoints. Wefindthatthehighcadenceandwidewavelengthrangeofthisdataisparticularlysuitedtoflarestudies, andrecommendthemforfutureobservingcampaignsinthenewsolarcycle.
WhatcanHinodeobservationstellusabouteruptionsfromsigmoidalactiveregions?
LucieGreen (UniversityCollegeLondon–MSSL)
SoftX-rayimagesoftheSunhaveshownthatsomeactiveregionscontainloops, orcollectionsofloops, whichappearforwardorreverse"S"inshape. Thesestructuresareknownassigmoidsandareofinterestbecausesigmoidalactiveregionshaveahighprobabilityofproducinganeruption. Recentobservationalandtheoreticalworkhassupportedtheinterpretationofthemagneticstructureofsomesigmoidsasbeingthatofafluxropelyingverylowinthesolaratmosphere, havingabaldpatchseparatrixsurfacetopology. Thisworkindicatesthatthefluxropeispresentinthesolaratmospherebeforetheonsetoftheeruption. Themainquestiontobeaddressednowishowthesigmoidalactiveregionswhichproduceaneruptionevolvetowardaninstabilityorlossofequilibrium.
WeuseHinodeobservationstoinvestigateeruptivesigmoidalactiveregions. Wediscusstheimportanceoftheevolutionofthephotosphericmagneticfield, theroleofreconnectionandpresentresultsfromEIS whichgiveaninsightintohowthesigmoidandoverlyingarcadefieldevolvetowardtheonsetofaneruption.
RegularizedinversiontechniquesforrecoveringDEMsfromHinode/XRT data
IainHannah (UniversityofGlasgow)withL. Braidwood, and E.P. Kontar
HinodeXRT providesunprecedentedspatialresolutionknowledgeoftheplasmatemperaturedistributionresultingfromheatinginthesolaratmosphere. However, theinferenceoftheDifferentialEmissionMeasureDEM(T) fromXRTrawdataisanill-posedinverseproblem. Here, wedevelopandapplyanenhancedmodel-independentregularizationalgorithmusedinRHESSI X-raysoftwareforthisprocessmakinguseofgeneralconstraintsontheformoftheDifferentialEmissionMeasures. Thealgorithmnaturallyprovidessignaldependentresolutionofthemethodthusgivingaclearcriteriatodeterminewhethertheplasmaisconsistentwithanisothermalmodel. Itcanalsobeeasilyadaptedtoworkwithothersolarmulti-filterdatasuchasSDO/AIA
WeshowbysimulationsthatthistechniqueyieldsDEM(T) withconsiderablymoreinformationandhigherqualitythanpreviousalgorithmsandapplythemethodtoXRT multi-filterobservationsofactiveregions.
Whatcantheorydoforyou?AlanHood (UniversityofStAndrews)
Analyticalapproximationsandnumericalsimulationsarefrequentlyusedtomodelvarioussolaratmosphericphenomena. Theseresearchtopicsareoftendrivenbythelatestobservations.A briefdescriptionofsomeoftheUK'srecentadvancesintheorywillbepresented, indicatingwherethedirectionthetopicsarelikelytotakeinthefuture. Theaimofthistalkistostimulateadiscussionofwhatobservationsareneededtodeveloptheoreticalmodelsfurther.
Coronalsignaturesofasunspotlight-bridgeSarahMatthews (UniversityCollegeLondon–
MSSL) with Deborah Baker, andSantiagoVargas Dominguez
Sunspotlight-bridgesarebrightlanesofmaterialthatdividetheumbra. Theirappearancesignifiesthereestablishmentofthegranulationwithinthespot, andoftenindicatesthebeginningoffragmentationofthespotitself. Theincreasedbrightnessofthelight-bridgerelativetothesurroundingumbraisaclearindicationthattheplasmatemperatureinthisregionishigher. Ithasalsobeennotedthatlight-bridgesoftenshowenhancedchromosphericactivity, withHα surgesandchomosphericjetsreportedinanumberofcases(e.g. Bhartietal. 2007, Shimizuetal.2009). Berger&Berdyugina(2003)alsofoundaconstantbrightnessenhancementabovealight-bridgeinobservationsinthe1600 ApassbandoftheTransitionRegionandCoronalExplorer(TRACE),whileKatsukawa(2007)foundthatlight-bridgeformationwasspatiallyandtemporallycoincidentwiththeheatingof ∼ 1 MK loopsasobservedbyTRACE.Light-bridgesthusseemtohavearoleinreleasingmagneticenergystoredinthespotaswellasinitsdecay. Inthisworkwe
48 P03–P04
useobservationsfromHinodeandSTEREO toinvestigatetheextenttowhichthepresenceofasunspotlight-bridgeaffectstheoverlyingtransitionregionandcorona. Inparticularwecommentonchangesinthecoronalvelocityfieldinconnectionwithactivityintheunderlyingphotosphereandcorona.
Relationshipbetweenmagneticfieldandcoronaloutflowsinactiveregions
RobertO'Neil (UniversityCollegeLondon–MSSL)with LouiseK. Harra, and DavidR. Williams
OutflowsfromtheedgesofactiveregionshavebeenobservedwithHinodeEIS.Itisexpectedthattheseoutflowsareoneofthesourcesoftheslowsolarwind. Thephysicalmechanismproducingtheoutflowsisasyetunclearwithvarioussuggestionsbeingputforward(e.g. compression(Murrayetal.), magneticreconnection(Harraetal.), quasi-separatrixlayers(Bakeretal.). Inordertoprogresstheunderstandingofoutflowsfurther,astatisticalstudyhasbeencarriedouttodeterminetherelationshipbetweenmagneticfieldandtheoutflowspeeds. Thisencompasseshowtheflowsevolvewithtime. Wewillpresentpreliminaryresultsanddiscusstheimplicationoftheserelatedtoslowsolarwindformation.
Activeregionmoss: basicphysicalplasmaparametersandtheirtimevariability
DurgeshTripathi (UniversityofCambridge)withHelen Mason, GiulioDel Zanna, and Peter Young
Wepresentastudyofthephysicalplasmaparameterssuchaselectrontemperature, electrondensity, columndepthandfillingfactorsinthemossregionsandtheirvariabilityoverashort(anhour)andalongperiod(5consecutivedays)oftime. Primarily, wehaveanalyzedthespectroscopicobservationsrecordedbytheExtreme-ultravioletImagingSpectrometer(EIS)aboardHinode. InadditionwehaveusedsupplementaryobservationstakenfromTRACEandtheX-RayTelescope(XRT).WefindthatthemossemissionisstrongestintheFexiiandFexiiilines. BasedonanalysesusinglineratiosandemissionmeasurewefoundthatthemossregionhasacharacteristictemperatureoflogT =6.2.TheelectrondensitiesmeasuredatdifferentlocationsinthemossregionsusingFexiiratiosareabout1-3×1010 cm(-3)andabout2-4×109
cm(-3)usingFexiiiandFexiv. Theelectrondensitysubstantiallyincreases(byafactorofabout3-4orevenmoreinsomecases)whenabackgroundsubtractionwasperformed. Thedensityandtemperatureshowverysmallvariationovertime. BycombiningtheobservationsrecordedbyTRACE,EIS andXRT,wefindthatthemossregionscorrespondtothefoot-pointsofbothhotandwarmloops.
ConvectiveplasmaaroundsolarporesSantiagoVargasDominguez (UniversityCollege
London–MSSL)
Magneticstructuresarecommonlyobservedinthesolarphotosphereatmanydifferentspatialscales,beingsunspotsandporesthemostconspicuousones. Theformation, morphologyandevolutionofmagneticfeaturesareintenselylinkedtosolaractivityfromthephotospheretothecorona.Convectiveplasmaandembeddedmagneticfielddeterminethedevelopmentofdifferentstructuresbutthereisnotclearconsensusfromamodelexplainingthetransitionfromporesintosunspots.Plasmaflowsinsolaractiveregionscangiveusaclueontheongoingprocessesandinteractions
leadingtotheformationofthesemagneticstructures, i.e. theformationofpenumbraearoundanumbralcore. Inthepresentworkwefollowtheevolutionofsolarporesfromhigh-resolutiontimeseriesofimagesbycomputinghorizontalpropermotions. Weaimatdeterminewhetherornotwefindevidencesofthepresenceofstronglargeoutflowsaroundpores, asinthecaseofsunspots,andhowtheplasmaflowsareaffectedintimebytheevolutionofthepores.
P05FRODOSpec: RoboticSpectroscopyusingthe
LiverpoolTelescopeRobertBarnsley (LJMU) with I.A. Steele
FRODOSpec(Fibre-fedROboticDual-beamOpticalSpectrograph)isanewbench-mounted,integralfieldunitspectrographcurrentlyavailabletousersofthe2mroboticLiverpoolTelescopeonLaPalma. I presentdetailsofthespectrographandalsotheautomatedpipelinereductionprocesswhichdistributestheresultingdatatotheend-userinanarrayofdifferentformatsincludingaonedimensionalarc-fittedspectrum. Weanticipatethattheautonomousnatureofthetelescopecombinedwiththeautomatedreductionprocedurewillbringnewdevelopmentsintheareasofrapidresponseastronomy, suchasGRBs,wherequickidentificationisessentialtoobtaininggoodqualityfollowupdata.
A studyoftheSuperWASP detectormapsJoaoBento (UniversityofWarwick)with
Peter Wheatley
TransitingplanetsurveyshavebecomeincreasinglypopularsincethefirstdiscoveryofaplanetarytransitaroundHD209458usingasmallandinexpensivewidefieldtelescope. Motivatedbythisresult, TheSuperWASP projectwasfounded, consistingof2robotictelescopesaimedatsurveyingthenightskyinsearchofplanetarytransits. Aswithmostgroundbasedsurveys,systematicnoiseisalimitingfactorinprecisionandagoodunderstandingofthisnoiseisvitaltoanypotentialimprovement. HerewepresentastudyoftheSuperWASP detectormaps,highlightingsomekeyfeaturesandinvestigatingtheircauses.
WhitherUK-LedGround-BasedSubmmAstronomy?
DavidClements (ImperialCollege)
TheUK hasagrandtraditioninground-basedsubmmastronomy, withahugelysuccessfulpastandwithgreatpotentialforthenextfewyearsthankstoSCUBA2. Beyondthistimescale, though,thereisnothingplannedwithclearUK leadership.I willreviewthepastandpresentandlookattherangeofpossibleopportunitiesforthisfieldinthefuture. Thispresentationisthenextstageinaprocessofcommunityconsultationonfacilitydevelopmentsforthefutureofthisfield.
JCMT andUKIRT:GoodNewsandBadNewsGaryDavis (JointAstronomyCentre)
ThetwoUK telescopesonMaunaKeahavehadcontrastingfortunesinthepastyear. UKIRT wasidentifiedfor"managedwithdrawal"bySTFC andIwillreportontheimplementationofthisandontheimplicationsforUKIDSS andotherongoing
programmes. TheJCMT,ontheotherhand, iscurrentlyinthemidstofacampaignofearlysciencewiththerevolutionarySCUBA-2instrumentandI willreportontheoutcomesofthiscampaign, thenear-termplansfortheJCMTLegacySurveyandthelong-termprospectsfortheobservatory.
e-MERLINSimonGarrington (UniversityofManchester)
e-MERLIN willprovide10-150milliarcsecondresolutionimagingatcentimetrewavelengthsandmicroJanskysensitivity. Thesecapabilitiesarevitalforresolvingkpc-scalestar-formingregionsandAGN indistantgalaxiesandAU-scaleprocessesofstar-formationinourGalaxy.Theenhancedsensitivityisbeingachievedwithnewbroad-bandreceiversanddedicatedopticalfibreconnectionstoanewcorrelator. Theinstrumentisbeingcommissionednowandsomeofthefirstresultswillbediscussed.
TheLiverpoolTelescope: ObservationswiththeSTILT (SmallTelescopesInstalledatLT) widefield
instrumentsNeilMawson (AstrophysicsResearchInstitute)
with Iain Steele
STILT isasetofthreewideimagingsetupsthathavetheabilitytoobservethousandsofobjectsinjustasingleimage. Thecurrentsetupincludes: anallskycamera, SkycamA,whichiscapableofimagingto6thmagnitudewhichshowsitiscapableofdetectingsomebrighttransientevents.A 20degreefieldofviewcamera, SkycamT,whichwithitswidefieldandtheabilitytoimageto∼ 12thmagnitudecanobservearound5000starsinasingleimageanda1degreefieldofviewtelescope, SkycamZ,whichiscapableofreaching18thmagnitude. SkycamZ alongwithSkycamT isattachedtothemainbodyoftheLiverpoolTelescopesobenefitsfromthepointingandtrackingabilityoftheLT.Allthreesetupscarryout10secondexposureseveryminute, soprovideconsiderableamountsofdatapernight. Theinstrumentshavebeenrunningforayearnowsothereisalsoanarchiveofunprocesseddatawhichcouldcontaindataonpasttransientevents. Theaimistocreateadatapipeline, whichwillautomaticallyreducethedataandcataloguetheobjectsineachimage. Thencrosscheckwithacurrentdatabaseandcreateanalertforanydetectedobjectwhichthesystembelievestobeofstellaroriginandpreviouslyuncatalogued. SofartheSTILT systemisalreadycontributingtotheanalysisofbothaGRB andanova.
EarlyresultsfromSCUBA2DavidNutter (CardiffUniversity)
Inthistalk, I willhighlightsomeoftheearlyresultsfromtheinitial'sharedrisks'observingperiodofSCUBA2ontheJCMT.InparticularI willshowdatafromtheJCMT GouldBeltSurveyofnearbystar-formingregions, anddetailhowthesedatawillbeusedtoimproveourunderstandingofthestar-formationprocess. Thequestionsthatweseektoanswerwiththesedataincludetherelationshipbetweenthemassfunctionofpre-stellarcoresatthelowestmasses, andtherelativelifetimesofthedifferentevolutionarystagesofstarformation. Iwillalsousesomefar-infrareddatafromtheAkarisatellitetodemonstratewhySCUBA2dataisessentialtocomplementthedatafromtheHerschelsatellite, andwhythelongwavelengthprovidedbySCUBA2, togetherwithshorterwavelengthdatafromHerschelwillbreakthe
P04–P05 49
degeneracybetweentemperatureandcolumndensity.
ALMA:statusreportandfirstscienceJohnRicher (Cambridge)with G Fuller, and
T Muxlow
ALMA isnowthelargestworkingsubmillimetreinterferometerintheworld: inDecember2009, itsfirstthree12-mantennasoperatedtogether, andphaseclosurewasachieved. Antennasandreceiverscontinuetoarriveandoverthenext3yearsALMA willgrowintoa66-elementarray.Thefirstcallforscienceproposalsislessthan12monthsawayinthecurrentschedule, andfirstsciencedatashouldbeavailableinlate2011. ThistalkwillsummarisethestateofALMAconstruction, andpresenttheexcitingscientificopportunitiesthatALMA willsoonenable.
HerschelandSPICA:pushingthefrontiersintothecoolcosmos
DimitraRigopoulou (STFC RAL/Oxford)
BuildingontheheritageofthesuccessfulHerschelmissionwillbeSPICA,ajointJAXA/ESA mission.ThisrepresentsamajorstepintheexplorationoftheDustyUniverseinthenextdecade. SPICA willpushthefrontiersonthephysicsofdustandtheinterstellarmediumfromplanetstothedistantUniversewithunprecedentedsensitivity- thankstoitbeingacryo-cooledmission. I willreviewthemajorscientificdriversofthemissionfocusinginparticularonsciencethatwillbecarriedoutwithSAFARI,theEuropean-ledfouriertransformspectrograph.
UpdateontheKMOS SpectrographforESO VLTRaySharples (UniversityofDurham)
KMOS isamulti-objectnear-infraredintegralfieldspectrometerunderconstructionbyaconsortiumofUK andGermaninstitutesfortheESO VLT.KMOS willbethefirstUK-ledfacilityclassinstrumentontheVLT andiscurrentlyinthefinalassembly, integration&testphase. ThistalkwillreviewthescientificpotentialofKMOS andshowtheresultsfromrecentprogressinthesubsystemmanufactureandtest.
P06TheMeerKAT DeepContinuumSurvey
MattJarvis (UniversityofHertfordshire)withKurtvander Heyden
I willpresentthecaseforalargecontinuumsurveytobeundertakenwiththeSouthAfricanSKA precursortelescope, MeerKAT.Scienceaimscovertheevolutionofstar-forminggalaxiesandAGN,cosmologyandlarge-scalestructureandtracingthemagneticfieldsintheUniverse.
EarlyresultsfromthecommissioningofLOFARJohnMcKean (ASTRON) with George Heald, and
LOFAR imagingcommissioningteam
TheLowFrequencyArray(LOFAR) willoperatebetween10and240MHz, andwillobservethelowfrequencyUniversetoanunprecedentedsensitivityandangularresolution. ThemainsciencegoalsofLOFAR aretoi)carryoutdeepextragalacticsurveys, ii)probetheepochofreionization, iii)studycosmicmagnetism, iv)investigatethetransientsky, v)studysolarphysics
andvi)observeultrahighenergycosmicrays.LOFAR willalsoprovideanimportanttestbedforthetechnologies(hardwareandsoftware)thatwillbeusedfortheSKA.
TheconstructionofLOFAR iswellunderway, withoverhalfoftheDutchstationsandthreeinternationalstationsroutinelyperformingbothsingle-stationandinterferometricobservationsoverthefrequencyrangethatLOFAR isanticipatedtooperateat. Here, I summarizethecapabilitiesofLOFAR andreportonsomeoftheearlycommissioningresults, concentratingonthewide-fieldimagingoftestfieldsaround3C 196and3C61.1between30-78MHzand120-168MHz.
RadioWeakGravitationalLensingwithVLA andMERLIN
PrinaPatel (InstitueofCosmology&Gravitation)with D.J. Bacon, R.J. Beswick, T.W.B. Muxlow, and
B. Hoyle
WecarryoutanexploratoryweakgravitationallensinganalysisonacombinedVLA andMERLINradiodataset: adeep(3.3micro-Jyperbeamrmsnoise)1.4GHzimageoftheHubbleDeepFieldNorth. I measuretheshearestimatordistributionatthisradiosensitivityforthefirsttime, findingasimilardistributiontothatofopticalshearestimatorsforHST ACS datainthisfield. Iexaminetheresidualsystematicsinshearestimationfortheradiodata, andgivecosmologicalconstraintsfromradio-opticalshearcross-correlationfunctions. I shallemphasizetheutilityofcross-correlatingshearestimatorsfromradioandopticaldatainordertoreducetheimpactofsystematics. UnexpectedlyI findnoevidenceofcorrelationbetweenopticalandradiointrinsicellipticitiesofmatchedobjects; thisresultimprovesthepropertiesofoptical-radiolensingcross-correlations. I exploretheellipticitydistributionoftheradiocounter- partstoopticalsourcesstatistically, confirmingthelackofcorrelation; asaresultI suggestaconnectedstatisticalapproachtoradioshearmeasurements.
A SETI pilotprogrammewithLOFARAlanPenny (U StAndrews)with M. Garrett
(ASTRON), M. Wise(ASTRON), R. Nichol(UPortsmouth), R. Fender(U Southampton), andH. Falcke(RadboudUniversiteitNijmegen)
TheLOFAR commissioningplanincludesapilotprogrammetoinvestigatetheuseofLOFAR forSETI observations. MostradioSETI searcheshavebeeninthe1-2GHzrange, andtheadventofLOFAR permitsdeepsearchesintherelativelyunexplored80-240MHzrange.
A fewnearbystarswillbesearchedfortheverynarrowbandemissionassociatedwithartificialsources, andthesensitivityofLOFAR anditsabilitytorejectterrestrialsourceswillbeinvestigated.Thisinvestigationwillhaveimplicationsforlow-frequencySETI workwithSKA.
PathwaytotheSKASteveRawlings (UniversityofOxford)
I willdiscussthesciencecasesforthevariouspathfinderandprecursortelescopesonthepathwaytotheSKA illustratinghowtheyinformonkeySKA science. TheseideaswillbeextendedtomapscienceoutputontothephasedconstructionoftheSKA itself.
P07Herschel: statusandin-orbitperformance
MattGriffin (CardiffUniversity)with ESA, SPIREconsortium, PACS consortium, and HIFI
consortium
ESA’sHerschelSpaceObservatorywaslaunchedinMay2009. Itisthefirstlarge-apertureFIR/submmspacemission, andthefirsttoextendbeyond200micronswavelength. Itcarriesa3.5-mdiametertelescope(thelargestastronomicaltelescopeyetflown), passivelycooledtoaround85K,andthreecryogenicallycooledscientificinstruments. PACS hasafarinfraredcameraoperatingat70, 100and160microns, andanimaginggratingspectrometercovering55–210microns. SPIRE hasathree-bandsubmillimetrecameraoperatingsimultaneouslyat250, 350and500microns, andanimagingFouriertransformspectrometercovering194–670microns. HIFI isaseven-channelsingle-pixelhigh-resolutionheterodynespectrometercoveringmostofthesubmillimetreregion. Thissuiteofinstrumentsallowsastronomerstocarryoutsensitiveimagingandspectroscopyoveradecadeinwavelength.HerschelhasbeenplacedinanorbitaroundtheSun-EarthL2point(aposition1.5millionkmdistantfromEarth, ontheanti-sunwardside), andwillhaveanoperationallifetimeofatleastthreeyears. Afterseveralmonthsofcommissioningandperformanceverification, thespacecraftandallthreeinstrumentsareperformingextremelywell.Manysuccessfulsciencedemonstrationobservationshavebeencarriedoutandroutineobservationsarenowunderway. I willdescribethemainfeaturesoftheobservatoryandtheperformanceandscientificcapabilitiesoftheinstruments.
SWIRE 70micronselectedGalaxies: FollowupandLuminosityFunction
HarsitPatel (ImperialCollegeLondon)withD.L. Clements
WepresenttheopticalandfarIR propertiesof70micronselectedgalaxiesfromtheSWIRE XMMLSSandLockmanfields. Wehaveobtainedspectroscopicredshiftsfor300newsourcesdownto70micronfluxlimitof9mJyand R < 22. Theredshiftdistributionpeaksat ∼ 0.3 andhasahighredshifttailouttoz=3.5. WeperformemissionlinediagnosticsforsourceswhereHα, Hβ, [NII]and[SII] emissionlinesareavailabletodeterminetheirpowersource. WefitsingletemperaturedustSEDs, Fν = Aβ
νB(ν, T ), to70micronsourceswith160micronphotometrytoestimatedusttemperaturesandmasses. Assumingadustemissivityindexof1.3wefindtemperaturesintherange ∼ 30 –50K anddustmassesintherange106–109 M⊙whichisconsistentwithresultsobtainedforSLUGS galaxies. Increasing βto2resultsinslightlycoldertemperatures, whichsuggesttheneedtoaccuratelydeterminetheshapeoftheRayleigh-JeanstailofthedustSEDandmoreimportantlytounderstandtheroleofcolderdust. TherecentlylaunchedHerschelsatellitewillshedlightontheseissues. WethenbuildfullSEDsforeachsourceusingthemultiwavelengthdatafromopticaltofar-IR.WefindinoursamplesourceswithIR luminositiesinrange108–1013 L⊙. TheSED fitsarethenusedtoconstructthelocal(z < 0.5)70micronluminosityfunctionandcompareourresultswiththeIRAS 60micronluminosityfunction.
50 P05–P07
FirstresultsfromtheDEBRIS surveyNeilPhillips (InstituteforAstronomy, UniversityofEdinburgh)with Jane Greaves, Brenda Matthews,Bruce Sibthorpe, Grant Kennedy, Laura Churcher,Amaya Moro-Martin, Mark Wyatt, and DEBRIS
consortium
TheDEBRIS surveyistargetingalargesampleofnearbymain-sequencestarsystems, exploitingthewavelengthcoverage, spacialresolutionandsensitivityofHerscheltodiscoverandcharacterisecooldebrisdiscs. HerewepresentfirstresultsofPACS 110and170micronsimagingoffivenearbyA andF typestarswithsignificantdustemission(βLeo, βUMa, ηCrv, ζTuc, ζDor). TheseobservationsarecomparedwithSpitzer/MIPS andJCMT/SCUBA imagesatshorterandlongerwavelengthsrespectively.
TheHerschel-ATLAS:A firstlookEmmaRigby (UniversityofNottingham)with H-
ATLAS team
TheHerschel-ATLAS isthelargestoftheHerschelSpaceObservatory'sopen-timekeyprogrammes.Itisalargeareaextragalacticsurveyprovidingsimultaneousfivebandphotometryacrossawavelengthrangeof110-500microns. TheareacoveredisfourtimesgreaterthanalltheotherHerschelextragalacticsurveyscombined, givingatotalcoverageof550squaredegrees. I willdescribethesurvey, andtheplannedscienceprogrammesassociatedwithit, andpresentthefirstresultsfromthesciencedemonstrationphaseobservations.
InitialresultsfromHerMES:theHerschelMulti-tieredExtragalacticSurvey
AnthonySmith (UniversityofSussex)withHerMES Consortium
HerMES,theHerschelMulti-tieredExtragalacticSurvey, isthelargest(900hour)guaranteed-timekeyprojectonHerschel, designedtocharacterizefar-infraredandsubmillimetregalaxypopulationsoverbroadrangesofredshift, luminosity, andenvironment. Targetfieldsrangeinsizeanddepthfromfractionsofasquaredegree, withdepthsbelowthesubmillimetreconfusionlimitforcharacterizingthegalaxiesthatcontributethebulkofthefar-infraredandsubmillimetreextragalacticbackground, totensofsquaredegreesforprobinglarge-scalestructureandtherelationoffar-infraredgalaxiestodarkmatter. A subsetofinitialresultsfromtheScienceDemonstrationPhasewillbesummarized, indicatingthehigh-redshiftscienceattainablewithHerschel. Areasofscienceinclude: measurementsofsourceconfusionnoiselevelsasafunctionofwavelength, galaxynumbercountsviadetectionstatisticsandfluctuationanalyses, galaxycolours, preliminaryspectralenergydistributionsandluminosityfunctionsforsamplesofgalaxies, andearlyimplicationsforgalaxymodels.
TheHerschelVirgoClusterSurvey(HeViCS)MatthewSmith (CardiffUniversity)with HeViCS
Consortium
TheHerschelVirgoClusterSurvey(HeViCS) isanopentimekeyprojecttoobserve64squaredegreesofthenearbyVirgoCluster. Theclusterwillbeobservedinparallelmodeprovidingdataat100, 160, 250, 350and500microns; whichcanbecombinedwithawealthofdataatotherwavelengths. I willdescribethemotivationforthesurvey, thescientificobjectivesandsomeofourfirstresultsfromsciencedemonstrationdata.
EarlyHerschelResultsonStarFormationDerekWard-Thompson (CardiffUniversity)with
J.M. Kirk, D. Stamatellos, and L. Wilcock
EarlyresultsfromHerschelarepresentedofanumberofstar-formingregions. Imagingat5wavebandsfrom70to500micronsallowopticaldepthandtemperaturemapstobemade. Coresonthevergeofformingstarsareidentifiedandmodelled. Someofthesearestarlesscores, someareprestellarandsomeareso-calledinfrareddarkclouds(IRDCs). FTS spectroscopyalsoallowsthegastobestudiedalongwiththedust. Typicalspectrashowthe12CO and13CO laddersoflines, aswellasCI.Weuseamonte-carlomodeltoobtainthephysicalparameterswithinIRDCsforthefirsttime. Theimplicationsfortheformationofhigh-massstarsarediscussed.
SPIRE FTS spectraofthreecarbon-richevolvedobjects
RogerWesson (UniversityCollegeLondon)withJ. Cernicharo, M. Matsuura, M. Barlow, L. Decin,
E. Polehampton, and MESS consortium
Lowtointermediatemassstarslosemostoftheirmassduringtheirfinalstagesofevolution, intheformofcool, lowvelocitywinds. Thismasslossisthedominantcontributortotheenrichmentoftheinterstellarmedium. Thepost-AGB objectsAFGL618andAFGL 2688, andtheplanetarynebulaNGC 7027areamongthebest-studiedcarbon-richevolvedsources, andISO observationsshowedthemtohaverichinfraredspectra. WehaveobtainedhighsignaltonoiseSPIRE FTSspectraofthesethreeobjects, coveringwavelengthsfrom200-670microns, apreviouslyunexploredregionofthespectrum. A largenumberofatomicandmolecularlinesfromawiderangeofspeciesaredetected; wepresentthesenewspectraandpreliminaryanalyses
P08Giantplanetmagnetospheres: JupiterandSaturnChrisArridge (UniversityCollegeLondon–MSSL)
ThemagnetospheresofJupiterandSaturnarethelargestandmoststudiednon-terrestrialmagnetospheresintheSolarSystem. Thevastsizeofthesestructuresispartlyduetostronginternaldynamosandlargeplanetarymagneticmoments,andpartlyduetotheirlocationintheheliospherewherethedynamicpressureofthesolarwindislowerthanthatneartheterrestrialplanets. Insidethejovianandkronianmagnetospheres, largeneutraltoriiformfromneutralssputteredandejectedfromthesurfacesoficyandvolcanicsatellites. Theseneutraltoriibecomeionised,producingplasmatorii. Thisplasmaisthensubjecttoaradialdiffusionprocess, knownasinterchange, whichspreadstheplasmathroughoutthemagnetosphere. Strongcentrifugalforcesassociatedwiththerapidlyrotatingplasmaconcentratethismaterialintoadisc. Outwardtransportandcouplingbetweentheplanet'sionosphereandequatorialmagnetospherealsoresultsinangularmomentumtransportbetweentheplanetandthemagnetosphericplasma. Inthistalktheconfigurationandequilibriumofthejovianandsaturnianmagnetosphereswillbereviewedandwillfocuson: magnetosphericstressbalance, magnetosphere-ionospherecouplingandthegenerationofplanetaryaurorae. Weshalldiscusstheeffectsofdipoletiltandsolarwind
forcingandhowtheseprocesses"break"theidealisednorth-southmagnetosphericsymmetry.Thetalkwillconcludewithcommentsonthecomparisonbetweengiantplanetandcooldwarfmagnetospheres.
Dynamicspectraofindividualradiopulsesinanultracooldwarf
GreggHallinan (UC Berkeley)
A numberofverylowmassstarsandbrowndwarfshavebeendetectedproducingperiodicpulsesofradioemission, whichhaveledtothesesourcesbeingdubbed"ultracooldwarfpulsars".OurbestevidencetodatesuggeststhisradioemissionisofthesamenatureasthatdetectedatkHzandMHzfrequenciesfromthemagnetizedplanetsinoursolarsystem, butrequiringmuchmorepowerfulkilogaussmagneticfields. Morerecently, periodicsignalsofthesameperiodasthosedetectedintheradiohavebeenfoundinopticalandinfraredphotometricandspectroscopicdataforanumberoftheseultracooldwarfpulsars. I willdiscusstheresultsofarecentArecibocampaignthatprovidesbroadbanddynamicspectraofindividualradiopulsesfromtheseobjectsaswellasamultifrequencyobservationinvestigatingtherelationshipbetweentheradiopulsesandthemysteriousperiodicsignalsdetectedinopticalandinfrareddata.
PhysicalParametersofUltracoolDwarfs: TheYoungandTheOld
RobertKing (UniversityofExeter)withMarkJ. McCaughrean, Jenny Patience,
Catia Cardoso, RobertDe Rosa, Derek Homeier,and France Allard
I willpresentourcomprehensivestudyofthephysicalpropertiestheoldfieldbrowndwarfbinary εIndiBa, Bb, thenearestbrowndwarfstotheSun, includingresultsfromhighangularresolutionoptical, near-infrared, andthermal-infraredimagingandmedium-resolution(uptoR∼ 5000)spectroscopyoftheindividualcomponents, andournear-completeastrometricmonitoringtodeterminethedynamicalsystemandindividualmassesofthesetwoT dwarfs. I willthendetailtheobservationsandinterpretationoftheyoung, low-massobject2M1207b, ayoungLdwarfwithanestimatedmassof ∼ 10MJup, butananomalouslylowluminosity. Thisobjectwillserveasakeycomparisonforupcomingnear-infraredspectroscopyofplanetsimagedaroundstellarhosts.
Finally, I willbrieflydiscusstheproblemsassociatedwithinferringphysicalpropertiesofultracooldwarfsfromlimiteddatasetsandthepossibilitiesforusinghighresolutionspectroscopicobservationsofultracoolbinariestoextractestimatesofthemetallicityfromsingleobjectsandso, inthelongerterm, investigateanydifferenceinheavymetalenrichmentwhichmayindicateformationthroughcoreaccretion.
Numericalsimulationoftheelectron-cyclotronmaserinstabilityinthemagnetospheresofbrown
dwarfsAlexeyKuznetsov (ArmaghObservatory)with
Gerry Doyle
Recently, anumberofbrowndwarfshavebeenfoundtobebrightradiosources. Theirradioemissionhashighbrightnesstemperature, highpolarizationdegree, andnarrowdirectivity. Theemissionisproducedmostlikelyduetotheelectron-cyclotronmaserinstabilityinaway
P07–P08 51
similartotheauroralradioemissionofthemagnetizedplanetsoftheSolarsystem. Inthiswork, wesimulatenumericallygenerationofradioemissioninmagnetospheresofbrowndwarfs. A2D codehasbeendevelopedtoinvestigatetheco-evolutionofanelectrondistributionandadistributionofmagnetoionicplasmawaves. Theinfluencesofaconvergingmagneticfieldandafield-alignedelectricfieldareconsidered, too. Thesimulationparameterswerechosenbasingonthemeasurementsintheterrestrialmagnetosphereandscaledtofittheexpectedconditionsatbrowndwarfs. Wefoundthatthedownward-directedaccelerationofelectronsbyfield-alignedelectricfieldtogetherwiththereflectionofparticlesfrommagneticmirrorresultinformationofthe"horseshoe"-likedistributions. Suchdistributionsareunstablewithrespecttoexcitationofdifferentmagnetoionicmodes, buttheZ-modeisdominant.AmplificationoftheZ-modewavesandtheelectrondiffusiononthemresultinarapidsaturationoftheelectron-cyclotronmaser, andthenthegrowthratesofallmodesdecreasesignificantly. Thefastordinaryandextraordinarymodesareneveramplifieduptothesaturationlevel. Ontheotherhand, thecontinuingactionofthefield-alignedelectricfieldandconvergingmagneticfieldpreventsthewave-particlesystemfromreachingacompletelysaturatedstate. Inparticular, thesefactorsareabletokeepthegrowthrateofthefastextraordinarymodeatthelevelsufficienttoproduceanintenseradioemission. Weusethesimulationresultstointerprettheobservations, andtoestimatetheparametersoftheemissionsources.
ThePeculiarbehaviourofRadioEmissioninFullyConvectiveStars
PaulineLang (UniversityofStAndrews)withMoira Jardine
LowMassStarshavebecomethesubjectofintensestudyasthesearchforexoplanetsbecomesmoreadvanced. M Dwarfsareofparticularinteresttousastheycanbethoughtofasthe'boundary'starsbetweenthesolar-typestarswithradiativecoresandconvectiveenvelopesandtheUltraCoolDwarfswhicharefullyconvective. InmainsequencestarsthereisadirectcorrelationbetweenX-rayluminosityandRadioluminosity.However, whenweentertherealmofthelowmassstarsthisrelationshipbreaksdown. Acrossthefully-convectiveboundarytheX-rayluminositychangeslittle, buttheradioemissionincreases; infactthelessmassivethestarthegreaterthiseffectbecomes. Workingundertheassumptionthattheradioemissioncouldbebeingproducedinanauroralring-likestructurenearthemagneticpoleofthestar, weaimtoreproducetheradiolightcurveseeninstarssuchasV374Peg.
UltraspecObservationsofTVLM 513-46546StuartLittlefair (UniversityofSheffield)
TVLM 513-46546isthebeststudiedoftheultracooldwarfpulsars; verylowmassstarswhichshowpulsedradioemissionontherotationalperiodofthestar. TheopticalvariabilityofTVLM513-46546presentsapuzzle. Itshowsperiodicvariabilityontherotationperiod, butmulti-bandobservationssuggesttheopticalvariabilityisdominatedbypatchydustcloudsinapredominantlyneutralatmosphere. Thisissurprisinginthecontextoftheradioemission.
HerewepresenttimeresolvedspectrophotometryofTVLM 513-46546usingtheelectronmultiplyingCCD,Ultraspec, takenaspartofa
multi-wavelengthcampaign. ThisdatasetallowstherelationshipbetweentheopticalvariabilityandtheHalphalinefluxtobeinvestigated,sheddingnewlightontheopticalvariabilityofTVLM 513-46546.
StructureanddynamicsoftheboundaryofSaturn'smagnetosphere
AdamMasters (UniversityCollegeLondon–MSSL) with N. Achilleos, A.J. Coates, and
M.K. Dougherty.
TheCassinispacecraft’sorbitaltourofSaturnallowsustostudytheboundaryofagiant,corotation-dominatedmagnetosphereintheoutersolarsystem. ProcessesoperateatthisinterfacebetweenthesolarwindandSaturn’smagnetospherethatleadtothetransportofmass,momentumandenergyintothesystem. TheresultsofasurveyofthecrossingsoftheboundaryregionmadebytheCassinispacecraftarepresented. Theorientationofthemagnetopausecurrentlayerisdeterminedforthemajorityofthecrossings. Ananalysisoftheboundarynormalssuggeststhatthecrossingsmadeduringanumberofspacecraftorbitsweretheresultofwaveactivityonthemagnetopausesurface. Thelow-latitudeinternalboundarylayerischaracterised. Variationsintheboundarylayerandthedependenceofthepropertiesofthelayerondifferentparametersareinvestigated. Thewiderrelevanceoftheseresultsformagnetosphericscienceisdiscussed.
VariationofSaturn'sUV aurorawithSKR phaseJonathanNichols (UniversityofLeicester)with
B. Cecconi, J.T. Clarke, S.W.H. Cowley,J.-C. Gerard, A. Grocott, D. Grodent, L. Lamy, and
P. Zarka
Itiswellknownthatvariouskronianmagnetosphericphenomenaexhibitoscillationsneartheplanetaryrotationperiod. However, theemittedUV auroralpowerhasnotbeenshowntovaryattheSKR period. Weuseanempirically-determinedSKR phasetoorderthe'quiettime'totalemittedUV auroralpowerasobservedbytheHubbleSpaceTelescopein2005, 2007, 2008and2009. OurresultssuggestthattheUV powerisapparentlydependentonSKR phase, althoughthepowervariationisonlybyfactorsoforder ∼ 2,ratherthantheordersofmagnitudeobservedintheSKR.Wealsoshowthatthevariationoriginatesfromthemorninghalfoftheoval, consistentwithpreviousobservationsofthesourceoftheSKR.
Sourceofperiodicradioemission; lessonsfromSaturn
DavidSouthwood (ESA) with M.G. Kivelson
ThepulsingradiosignalsfromSaturn(Saturnkilometricradiation, SKR),yieldsomeinterestinglessonsforboththeproblemofidentifyingtheultimatesourceoftheradiosignalbutalsoonwhatmaybededucedfromperiodicradioemissioningeneral. Commonlyithasbeenthoughtthatperiodicradioemission, becauselinkedtothemagneticfieldyieldsdirectinformationonthedeeprotationofanobject.WhatisknownfromSaturndrawsthisassumptionintodoubt. WereviewwhatisknowntherelationbetweentheSaturnemissionandtheplanetarymagnetosphericmagneticfieldaftersixyearsofCassinispacecraftorbitaldata. TheSKR isgeneratedastheby-productofaninternalinteractioninthemagnetosphere. Theperiodicsignalisinpracticepulsedandyetlinkedtoarotatingmagneticstructure. Theprimaryinteractionisaresultofthemodulationoffield-
alignedcurrentsgeneratedbetweentheoutermagnetosphericfieldwhereitisstressedbythesolarwindandarotating“cam”magneticfieldstructurewhichisthedominantfieldperturbationintheinnerandmiddlemagnetosphere.
InfluenceofupstreamsolarwindconditionsonatmosphericflowsatJupiter
JaphethYates (UniversityCollegeLondon)withNicholas Achilleos, and P. Guio
ThecouplingofJupiter'smagnetosphereandionosphereplaysavitalroleincreatingitsauroralemissions. ThestrengthoftheseemissionsissomewhatdependentontherelativerotationalflowswithinJupiter'sthermosphereandthemagnetodisc. Usinganazimuthallysymmetricglobalcirculationmodel, wewereabletosimulatehowup-streamsolarwindconditionsaffectatmosphericflows; herewepresentthesepreliminaryestimates. Wecalculatedmagneticfieldprofilesrepresentingcompressedandexpandedmagnetospheres, andtheseprofileswerethenusedtogainfurtherinsightonthemagneticconfigurationandcouplingofthemagnetospherewiththeionosphereandhowthiseffectsglobalwindsandenergyinputswithinJupiter'sthermosphere.
Mappingradioemitting-regiononlow-massstarsandbrowndwarfs
ShenghuaYu (ArmaghObservatory)withJ.G. Doyle, G. Hallinan, A.L. MacKinnon, and
A.E. Antonova
A numberofrecentradioobservationsindicatemagneticactivityoperatedbydynamotheorywouldbecommonphenomenononultracooldwarfs(UCDs, spectralclasseslaterthanM7).Currently ∼ 11 radioactiveUCDsareshowingveryhighbrightnesstemperatureandhighly(upto100%)circularpolarization, including3withstrongperiodicradiobeams. Thenatureoftheemissioncouldbeinterpretedbyaneffectiveamplificationmechanismofthehigh-frequencyelectromagneticwaves- theelectroncyclotronmaser(ECM) instability. Wehaveperformedone-dimensionalparticlesimulationtoinvestigateresponseofweaklyrelativisticelectronbeamstoamagnetic-field-alignedelectricfieldinducedbyatime-varyingexternalcurrentsource. Wefoundrelativisticelectronbeamscouldresultinstrongerinstabilitythannonrelativisticbeams. Bythesimulation, weareabletodeterminethesizeandheightofradioemitting-region, electrondensity,timescaleoftheinstabilityandevensurfacemagneticfieldofUCDs.
P09Determinationofthephotometriccalibrationandlarge-scaleflatfieldoftheSTEREO Heliospheric
Imagers: I.HI-1DanielleBewsher (JeremiahHorrocksInstitute,UCLan)with D.S. Brown, C.J. Eyles, B.J. Kellett,
G.J. White, and B. Swinyard
Theaimofthispaperistocalculateanaccuratelarge-scaleflatfieldfortheSTEREO HI-1instruments. ThisisdonebyanalysingthevariationinintensityofstarsinthebackgroundstarfieldastheypassacrosstheCCD.Inordertousethebackgroundstarfield, aphotometriccalibrationisperformedwhichdefinesaHImagnitudescaleandaconversionbetweenthis
52 P08–P09
scaleandmeasuredintensity. Thephotometriccalibrationusesstellarspectrafoldedthroughtheinstrumentresponsetomakeinitialintensitypredictions. However, asecondarypredictionmethodbasedonthephotometriccalibration,whichblendstheR-, V- andB-magnitudesofastar, isderivedforstarswithnospectralinformation. Inaddition, asolarspectrumfoldedthroughtheinstrumentresponseisusedtodetermineconversionfactorstoconvertfromHIintensityunitsintomeansolarbrightness, S10andSI units, fordiffuseorextendedsources.
TheRosettaPlasmaConsortiumChrisCarr (ImperialCollegeLondon)with
Elizabeth Lucek
TheRosettamissionisoneoftheoriginal‘cornerstone’missionsofESA’sHorizons2000scienceprogramme. Thespacecraftwaslaunchedin2004, willrendezvouswiththecomet67PChuryumov-Gerasimenkoin2014, followthecometfromdeep-spacethroughtoperihelion, andplacealandercraft(Philae)onitssurface.Consequently, Rosettawillallowbothremotesensingandinsitumeasurementssimultaneously.Cometscontainthemostpristine, least-processedmaterialinoursolarsystem. Thereareprobablyevenpre-solargrainspreservedinsidethesebodies. TheaimofRosettaisnothinglessthantounderstandtheoriginsofthesolarsystem. Rosettaappealstotwodistinctcommunities: theplanetaryandsolarsystemscientistswhowillinterpretcometsasthebuildingblocksofthesolarsystem,andthespacescientistswhoareconcernedwiththegas/dust/plasmainteractionwiththesolarwind. Forboth, thecometisanaturallaboratorywhichwouldbeimpossibletore-createontheground. RosettahastheopportunitytobringthesestrongUK communitiestogether, furthermorethereisplentytointerestastronomerstoo. TheRosettaPlasmaConsortium(RPC) isasuiteofinstrumentationontheorbiterspacecraftdedicatedtounderstandingtheevolutionofthecomet/solar-windinteractionasafunctionofheliocentricdistance(andhencecometaryactivity). InthisposterweoutlinethescientificpossibilitiesoftheRPC meaurements. Wedescribethecapabilitiesoftheinstrumentsuiteandtheexpectedenvironmentinwhichtheywilloperate.
EuropaJupiterSystemMissionMicheleDougherty (ImperialCollegeLondon)
TheEuropaJupiterSystemMission(EJSM) isaninternationalmissiontotheJupitersystemwithjointparticipationfromESA andNASA.ItconsistsoftwoprimaryflightelementsoperatingintheJoviansystem: theESA-ledJupiterGanymedeOrbiter(JGO) andtheNASA-ledJupiterEuropaOrbiter(JEO).JGO andJEO willexecuteanextendedchoreographedexplorationoftheJupiterSystembeforesettlingintoorbitaroundGanymedeandEuropa, respectively. TheoverarchinggoalofEJSM isthestudyoftheemergenceofhabitableworldsaroundgasgiants. JGO andJEO willcarrycomplementaryinstrumentstoachievethefollowingscienceobjectives: characterizeGanymedeandEuropaasplanetaryobjectsandpotentialhabitats, studyGanymede, Europa,CallistoandIointhebroadercontextofthesystemofGalileansatellitesandfocusonJupiterscienceincludingtheplanet, itsatmosphereandthemagnetosphereasacoupledsystem.
SOHO CoronalDiagnosticSpectrometerAndrzejFludra (STFC RutherfordAppleton
Laboratory)with Andrzej Fludra(STFC RutherfordAppletonLaboratory)
TheSolarandHeliosphericObservatory(SOHO),launchedinDecember1995, hasbeeninoperationforover14years. TheCoronalDiagnosticSpectrometer(CDS) isaUK-ledinstrumentonboardSOHO,operatedbyateamfromtheRutherfordAppletonLaboratory. TheCDS facilityhasbeenusedextensivelybyalargeusercommunity, including15UK researchgroupsandover60groupsworld-wide, andsciencestudiesfill24hourseachday. CDS continuestobeusedforallaspectsofsolaratmosphericresearchthatcanbestudiedfromEUV spectra,participatinginregularobservingcampaignswithHinodeandSTEREO spacecraft. Recenthighlightsincludenewactiveregionloopsanalysis, newresultsonexplosiveandgentlechromosphericevaporationduringflares, spatiallyresolvedanalysisofactiveregionheatinginthetransitionregionemission, andjointobservationsofHeliumlinesbythreespectrometers(CDS,SUMER andEIS) thatrevisethelong-standingproblemofenhancedHeliumlineintensities. CDS remainstheonlyspectrometerobservingstrongspectrallinesfromseveralspecies, includingionsofFe, Si,Al, Mg, Ca, Ne, N,O,andHe. Bright, unblendedlinesatcooler, transitionregiontemperaturesareuniquetoCDS andprovidemeasurementsofDopplervelocitiesofthecoolfilamentmaterialassociatedwithnearlyalleruptionsleadingtoCoronalMassEjections, throughlinesofHeI andO V.CDS willthusbetheonlyavailablesourceofspectroscopiccharacterisationoftheunderlying,coolplasmainvolvedineruptiveeventsandCMEsobservedwiththeSolarDynamicsObservatoryAIA fromApril2010. JointCDS andSDOobservationswillbealsovitalforstudiesofthermalstructureandheatingofloopsinthequietsunandactiveregions, thesolarEUV irradiance,andin-flightcalibrationofthespectralresponseoftheSDO AIA bands.
Scienceopportunitiesforgeospacestudies?MikeHapgood (STFC RutherfordAppleton
Laboratory)
Thenear-Earthspaceenvironmentisanimportanttargetforscientificresearcharoundtheworld. Itsdifferentregions(ionosphere/thermosphere,plasmasphere, radiationbeltsandmagnetosphere)exhibitmanyphysicalprocessesthatchallengeourunderstanding, thatareoftenofpracticalimportanceandthatareexemplarsofprocessesthatoccurinmanyotherastrophysicalenvironments. ThistalkwilloutlineanumberofcurrentandfutureopportunitiestostudytheseregionsandexplorehowUK scientistscanexploitthoseopportunities.
TheSTEREO MissionRichardHarrison (RutherfordAppletonLaboratory)
with C.J. Davs, J.A. Davies, C.J. Eyles, andS. Crothers
WeprovideastatusreportontheNASA STEREOmissionandinparticularontheUK-ledHeliosphericImagerinstruments, includinganupdateofrecentscientificresults.
SuperDARN UK:A newresourcetostudyoftheupperatmosphere
MarkLester (UniversityofLeicester)withG. Chisham, M.P. Freeman, S.E. Milan, J.A. Wild,
and T.K. Yeoman
TheSuperDualAuroralRadarNetwork(SuperDARN) hasprovidedobservationsofthepolar, auroral, andsub-auroralionosphereinbothhemispheresforthelast16years. TheUK hasplayedacentralroleintheinitialdevelopmentofSuperDARN andinitsexpansionthroughtheconstructionandoperationsofradarsatHalleyAntarctica, fundedbyNERC,andinFinlandandIceland, fundedbyPPARC andSTFC.FurthermoretheUK hasbeenoneofthemajorusersofthedatafromthenetwork. WiththemoveofgroundbasedSTP fromSTFC toNERC,thewholeoftheUK'scontributiontoSuperDARN comesundertheremitofNERC.Recently, ajointprogrammebetweentheBritishAntarcticSurvey(BAS) andtheUniversityofLeicesterhasseenthedeploymentofaradarontheFalklandIslandsspecificallytoinvestigatetheupperatmosphereinthatregion.AninitiativebeingdevelopedbyBAS,theUniversityofLeicesterandLancasterUniversitywillprovideanewUK facility, SuperDARN UK,whichwillenabletheUK atmosphericcommunitytohave(i)directaccesstocontinuousregionalsynopticandclimatologicalmeasurementsofwinds, wavesandtidesintheNorthandSouthAtlanticsectorupperatmosphere, andofenergyinputsfromSpace; (ii)opportunitiestoruntheirownupperatmosphereexperimentsononeormoreradars, forupto50%ofthetotaloperationaltime; (iii)immediatehigh-leveldataproductsfromthewiderSuperDARN network; (iv)usersupportforSuperDARN dataanalysissoftwareandexperimentdesign; and(v)trainingopportunitiesforstudentsinradartechnologyandatmosphericscienceexperiments. Inthispresentationwegiveanoverviewofthesystem, thedataproductsavailableandthesciencewhichcanbeachievedwithSuperDARN.
ClusterFGM:currentandfuturescientificopportunities
ElizabethLucek (ImperialCollege)with C.M. Carr
Theuniquefour-point, multi-instrumentmeasurementsmadebytheClusterspacecraftovernearly10yearshavealreadyrevolutionisedourunderstandingofthedynamicsofspaceplasmaphysicsprocesses. However, therecentextensionofthemissionuntiltheend2012, togetherwiththeevolutionofthespacecraftorbittocrossnew,asyetunexploredregionsofthemagnetosphere,promisethatdiscoverieswillcontinuetobemade.TheopportunityforscientificprogressisalsosupportedbytheunprecedentedwealthofhighqualityandhighresolutiondatafromallClusterinstruments, availabletoallscientiststhroughtheESA ClusterActiveArchive. Inthepastfewyearsthesatelliteorbithasevolvednaturally, andmeasurementshavealreadystartedtobemadeintheauroralaccelerationregion. Anotherproductiveareahasbeenincollaborationswiththe5THEMIS spacecraftlaunchedbyNASA.Inthenearfutureadditionalkeysciencetargetswillbemeasurementsofcurrentdisruptioninthetail;samplingthepartialringcurrentanditsconnectionwithmagnetosphericcurrentsystems;measurementoftheradiationbeltsandtheinnerplasmasphere; andconjunctionswithSWARM:3satellitesscheduledforlaunchbyESA in2011tomakecomprehensivemeasurementsofthestrength, directionandevolutionoftheEarth’sfield. Finally, anewinitiativetoopenupCluster
P09 53
sciencetothewiderscientificcommunityhasbeenmadebymakingacallforscienceproposalsfor“specialorbits”, allowinginstrumentoperationstobetailoredtoaparticularscientifictarget, Thenewemphasisonmeasurementsoftheinnermagnetospherepresentchallengesforthemagnetometer, asthemagneticfieldmagnitudeexceedsourexpectedoperatingrange. Inthisposterweconsidersomeoftheforthcomingscientificopportunities, andsummarisethestatusofFGM calibrationsanddataavailability.
SolarOrbiter: exploringtheSunandHeliosphereconnection
RichardMarsden (ESA)
UnderstandingtheconnectionsandthecouplingbetweentheSunandtheheliosphereisoffundamentalimportancetoaddressingoneofthemajorscientificquestionsoftheESA CosmicVision2020programme: "HowdoestheSolarSystemwork?"Theheliospherealsorepresentsauniquelyaccessibledomainofspace, wherefundamentalphysicalprocessescommontosolar,astrophysicalandlaboratoryplasmascanbestudiedunderconditionsimpossibletoreproduceonEarth, ortostudyfromastronomicaldistances.TheresultsfrommissionssuchasHelios, Ulysses,Yohkoh, SOHO,TRACE andRHESSI,aswellastherecentlylaunchedHinodeandSTEREOmissions, haveformedthefoundationofourunderstandingofthesolarcorona, thesolarwind,andthethree-dimensionalheliosphere. Eachofthesemissionshadaspecificfocus, beingpartofanoverallstrategyofcoordinatedsolarandheliosphericresearch. However, animportantelementofthisstrategyhasyettobeimplemented.NoneofthesemissionshavebeenabletofullyexploretheinterfaceregionwherethesolarwindisbornandheliosphericstructuresareformedwithsufficientinstrumentationtolinksolarwindstructuresbacktotheirsourceregionsattheSun.ThisistheoverarchinggoalofSolarOrbiter. Withpreviouslyunavailableobservationalcapabilitiesprovidedbythepowerfulcombinationofin-situandremotesensinginstruments, andtheuniqueinner-heliosphericmissiondesignspecificallytailoredforthetask, SolarOrbiterwilladdressthecentralquestionofheliophysics: HowdoestheSuncreateandcontroltheheliosphere? Inthispaper, wewillpresentthedetailedsciencegoalsofthemissionandbrieflyreviewitsstatus.
SolarOrbiter: TheSolarWindAnalyserInvestigation
ChristopherOwen (UniversityCollegeLondon–MSSL) with D.O. Kataria, B.K. Hancock,
A.N. Fazakerley, C. Brockley-Blatt, P. Louarn,S. Livi, and R. Bruno
SolarOrbiterwillexploreinnermostheliospheretounravellinksbetweenactivityinthemagneticfield-dominatedregimeofthesolarcoronaandtheirconsequencesintheparticle-dominatedregimeoftheinterplanetarymedium. TheselinkswillberevealedthroughanalysisofobservationsoftheSunfromacomplementofpowerful, high-resolutionopticalinstruments, togetherwiththosefromstate-of-the-artinstrumentswhichsample, insitu, theproperties, dynamicsandinteractionsofplasma, fieldsandparticlesinthenear-Sunheliosphere. Inaddition, theseplasmaandfieldinstrumentshavehightemporalresolutions, andthusofferuniquepossibilitiesforresolvingplasmakineticprocessesatintrinsicscales.
Inordertoachievethemissionsciencegoals, weneedhigh-cadencemeasurementsof3D velocity
distributionfunctionsofthesolarwindelectron,protonand α−particlespopulations, abundantheavyionssuchasO6+andlowironchargestatessuchasFe9+orFe10+. ThesemeasurementsareamongthosethatwillbemadebytheSolarWindAnalyser(SWA) suiteonSolarOrbiter. Thisinvestigationrequiresmajorinternationalhardwarecollaborations, butisledbytheUK (P.I.institute: UCL/MullardSpaceScienceLaboratory).Inadditiontotheoverallleadershipofthesuite,UCL/MSSL willprovidethebulkofthehardwarefortheElectronAnalyserSystem, oneof3sensorsystemswithinthesuite. TheProton-AlphaSensorandtheHeavyIonSensorareledbypartnersinFranceandtheUSA respectively, whileacentraldataprocessingunit, tobebuiltinItaly, servesall3sensorsandcompletesthesuite.
Inthisposterwebrieflypresentthesciencegoalsrelatedtotheinsituexplorationoftheinnerheliosphereand, inparticular, weaddresstheSWA sensordesignsrequiredtomeetthesegoalsunderSolarOrbiterschallengingmeasurementenvironment.
HinodeUnveilsA NewSunJianSun (UniversityCollegeLondon–MSSL) with
Louise Harra, David Williams, Len Culhane,Lucie Green, and Deb Baker
HinodeisajointJapan/UK/US missionwithESAandNorwegianinvolvement. Usingacombinationofoptical, EUV andX-rayinstrumentationHinodewillstudytheinteractionbetweentheSun'smagneticfieldanditscoronatoincreaseourunderstandingofthecausesofsolarvariabilityandtheoriginsofsolaractivity. HinodewaslaunchedsuccessfullyinSeptember2006.
Thispostergivesanoverviewofthethreeinstrumentson-boardtheHinodespacecraft: SolarOpticalTelescope(SOT),X-RayTelescope(XRT)andEUV imagingspectrometer(EIS).Severalsignificantobservationalresultsobtainedduringthefirst3.5yearsofmissionoperationsarealsopresented.
NASA SDO,itsscienceandtheUCLandata-hubRobertWalsh (UniversityofCentralLancashire)
with S. Dalla, D. Bewsher, B.J.I. Bromage,D.S. Brown, S.A. Chapman, M. Marsh, J. Pearson,
C. Alexander, and J. Kelly
LaunchedonFebruary11, 2010, theSolarDynamicsObservatory(SDO) willrevolutioniseourunderstandingoftheSunwithitsexcellenttemporalresolutionandcontinuousfulldiskcoverage. Thispresentationwillhighlightthescientificaimsofthemissionandhowitsthree-instrumentsuitewillprovideawealthofopportunitiesfornewdiscoveries. Inparticular,wewillemphasizethechallengesassociatedwiththeapproximateterabyteperdaysizeofthedatasetandwillpresenttheSDO/AIA datahubbeingsetupattheUniversityofCentralLancashire. Further, wewilloutlinehowtheUKsolarcommunitywillbeabletointeractwiththehubintheverynearfuture.
P10TheWFCAM ScienceArchive
RobBlake (RoyalObservatoryEdinburgh)withNigel Hambly, Eckhard Sutorius, Mike Read,Nick Cross, Ross Collins, Mark Holliman, and
Peredur Williams
InfraRedDeepSkySurveysoftheNorthernHemisphere
TheWFCAM ScienceArchive(WSA) isamature,databasedriven, webaccessibleproductprovidingaccesstodatatakenbytheWFCAM instrumentonUKIRT aspartoftheUKIRT InfraRedDeepSkySurveys(UKIDSS).
Thedataareavailableaspixeldata(inmulti-extensionFITS files), jpegimages(includingcolourimageswhereavailable), aswellasfullyqueryablerelationaldatabasescontainingfullinformationonalldetections.
AswellasUKIDSS data, theWSA alsocontainsneighbourtablesrelatingUKIDSS detectionstothoseofothersurveys(including2MASS,2XMM,MGC,andsixdatareleasesfromtheSloanDigitalSkySurvey). Forconvenience, alloftheseexternalcataloguesarealsoavailabledirectlythroughtheWSA interfacesothatdetectionscanbeinstantlyqueriedinallsurveys.
February2010sawtheseventhUKIDSS datarelease(DR7)containingover105millionsourcescoveringover3,000squaredegreesacrossthreeofthesurveys(theLargeAreaSurvey, GalacticClustersSurvey, andDeepExtragalacticSurvey)withdepthsofuptomagnitude22.4. A further770millionsourcescoveringover1,300squaredegreesareduetobeaddedshortlywiththeadditionoftheGalacticPlaneSurvey(GPS) intoDR7.
WepresentanoverviewofthelatestfeaturescontainedinDR7whichareavailabletoregisteredusers, aswellascoveringthefeaturesnowaccessibletoeveryoneinourlatestworldrelease(DR4).
DataIntegrationinHeliophysicsJohnBrooke (UniversityofManchester)with
Anja LeBlanc
HeliophysicsisarelativelynewdisciplinethatexplorestheSun-SolarSystemConnection.Althoughtheindividualcommunitiesinvolvedinheliophysicsarewellestablished, theyhaveevolvedindependentlyandcurrentlyitisextremelydifficulttofindandcomparedatafromacrossthediversesetofexistingdataarchives. WedescribetheuseofmethodsderivedfromtheSemanticWebtoaddressthisproblem. Wehaveintegrateddescriptionsofdatatodevelopanabstractheliophysicsdomainontology, whichcanbethoughtofasacontrolledvocabularyenrichedwithrulesthatcanbereasonedaboutbymachines. Theaimofthisontologyisbeusedtomapdata(describedbydatamodels)fromdifferentregionsoftheheliosphere. Wearealsodevelopinganontologyforcoordinatesystems,whichcandeterminewhethercoordinatesystemscanbetranslatedintoeachotherandifso,whetherthetimeisaparameteroftheoperation.Wealsodescribeworkflowswhichuseanontologytofindrelevantdatasets, e.g. whichusesanabstracttermsuchas"flare"toquerydatasetsfromtheHESSI flarelist, YOKOH flarelist, KSOflarelist. Theworkflowfindsoverlappingevent
54 P09–P10
datafromdifferentsources, itfindstherelevanttimeintervaandlooksuptheeventlist, andcheckswhetherallinstrumentshavedatatothiseventandreturnsonlyeventsanddatawhichoverlapeachother. ThisworkispartoftheHELIOprojectfundedbytheEU intheFP7programme,seehttp://www.helio-vo.eu/
TheSuperWASP publicarchiveOliverButters (UniversityofLeicester)with
R.G. West, D. Pollacco, C. Hellier, A.C. Cameron,and WASP Consortium
TheSuperWASP (WideAngleSearchforPlanets)projectistheworld'sleadingtransitingexoplanetsurvey. Itconsistsoftworoboticobservatories(oneintheNorthernhemisphereandtheotherintheSouthernhemisphere)thatconstantlymonitorthenightsky. Imagesaretakensimultaneouslyfromeightwide-anglecamerasineachcase. Datafirststartedtobetakenin2004, sincethenthedatasethasbeenextensivelysearchedfortransitingexoplanets. Other(nonexoplanet)sciencehascomefromthedataalso, suchasthecorrelationofROSAT sourceswithvariablestarsandasteroidstudies, butthereisstillawealthofothersciencethatcanbedonewiththedata. WiththisinmindweannouncethefirstpublicdatareleaseoftheSuperWASP archive.
Thisfirstdatarelease(DR1)startsin2004intheNorthand2006intheSouthandstretchesto2008inbothcases. Thiscorrespondstojustunderfivemillionimages, each7.8x7.8degrees. Fromtheseimagesover100billiondatapointshavebeenextractedforover20millionuniqueobjects. TheSuperWASP publicarchivemakesallthisdatasearchableanddownloadableviaawebinterfacehostedattheUniversityofLeicester.
VOeventstriggeredbygravitywavesTobiaCarozzi (Univ. ofGlasgow)with
Norman Gray, and Graham Woan
VirtualObservatoryevents(VOevents)areXMLbasedmessagesthatdescribeastronomicalevents.TodatedespitethediversityofVOevents, rangingfromsupernovaeto γ−raybursts, theyhaveallbeenofelectromagneticorigin. Inthiswork, welookathowtheVOeventframeworkcanalsobeuseddescribeeventsofagravitionalorigin. WealsolookathowVOeventscanbepropagatedfromtheLIGO-VirgoAlertSystemtoVOeventsubscribersusingtheExtensibleMessagingandPresenceProtocol(XMPP).
NativeSyntheticImagingofSmoothedParticleHydrodynamicsSimulations
DuncanForgan (SUPA,IfA,UniversityofEdinburgh)with Ken Rice
I willpresentanewnumericalmethodforcreatingsyntheticobservablesfromSmoothedParticleHydrodynamics(SPH) simulations. ItemploysMonteCarloRadiativeTransfer(MCRT) techniquestoemulatethetransmissionofphotonsthroughamedium, incorporatingbothabsorptionandscattering, capturingthemonanimageplaneinamanneranalogoustothecaptureofphotonenergyonaCCD.
UnlikepreviousattemptsatimagingSPH fields, Iemployraytracingtechniquesthatdonotrequiregridding, preservingthesimulation'snativeresolvingpower. Thecodealsousesalgorithmsoriginallydevelopedforcomputergraphicsproblemstooptimiseitsefficiency.
ThismethodthereforeprovidesadirectlinkbetweenSPH simulatorsandobservers, allowingmoreconcreteobservationalpredictionstobemade. I willillustratethisbyimagingSPHsimulationsofprotostellardiscsystemstodeterminewhatfeaturescanberesolved, e.g. discspiralarmsorembryonicprotoplanets.
NewinfraredandopticalimagesservicesintheVO
NigelHambly (UniversityofEdinburgh)withM.S. Holliman, M.A. Read, and R.G. Mann
ThisposterdescribesnewSimpleImageAccess(SIA) servicespublishedtotheVirtualObservatorybytheWideFieldAtronomyUnitattheInstituteforAstronomy, UniversityofEdinburgh. Intheinfrared, weprovideimagesfromthelatestreleasesfromUKIDSS,including1000sofsquaredegreesfromthewide-angle, shallowsurveysin1.0to2.5micronpassbands(YJHK).Intheoptical,weprovideanall-skySIA cut-outservicebasedonthelegacySchmidttelescopephotographicsurveys(epoch1949-2000)asdigitisedbythenowdecommissionedprecisionplatescanningfacilitySuperCOSMOS.EverypartoftheskyiscoveredinBRI withatleasttwoepochsinR;multiple-epochimagesareavailableinthesubstantialsurveyoverlapregions. Furthermore, specialistregionshaveadditionalfilter/epochcoverage, e.g. HalphaandmatchedR exposuresintheGalacticPlane,andaround200multi-epoch/colourimagesspreadover30yearsintheESO/SRC surveyfield287at21h28m, -4500(B1950).
TheseserviceshavebeenpublishedtotheVOthroughtheWFAU publishingregistry, whichcanbefoundthroughtheIVOA RegistryofRegistries.
VirtualObservatoryServicesatWFAUMarkHolliman (UniversityofEdinburgh, Institute
forAstronomy)with Mike Read
TheWideFieldAstronomyUnithostsanumberofVirtualObservatory(VO) servicesthatenableaccesstobothdataandprocessingapplicationshousedonourserversinEdinburgh. Theseservicesprovideastronomerswithapowerfulsetoftoolsforobtainingandprocessingdatainwaysunattainablethroughconventionalaccessmethods. TheservicesofferedincludeconesearchandADQL accesstoanumberofmajordatabasesdevelopedbyourdatacentresuchasUKIDSS,SuperCOSMOS ScienceArchive, andthe6dFGalaxySurvey, andalsomanymirrorsofimportantdatabasesdevelopedelsewhere, suchasSDSS,IRAS,and2XMM .ImagesforUKIDSS andSuperCOSMOS areaccessiblethroughSIAservices. ThereareusefuldataprocessingtoolsliketheSTILTS libraryfortablemanipulation, adataminingtoolforclassificationusingkerneldensityanalysis, andaserviceforconvertingVOTablesintoKML foruseinGoogleSky. AlsohostedareanumberofVO infrastructureserviceslikeafullregistryandVOSpacethatenableuserstofindresourcesandstoredatainanonlineaccessiblelocation. WFAU providessecuredVOservicestotheproprietaryUKIDSS releases, whicharethefirstsecuredVO servicesforamajorproprietarydataresourceintheentireVO.WithalimitedknowledgeofpythonandacopyoftheVODesktopsoftwareastronomerscanscriptupworkflowsthatutilizetheseservicestoperformcomplexoperationslikecrossmatchingbetweendisparatedatasetsorextractingcataloguesfromimagesremotely. Sincemanyofourdatabasesaretoolargetobedownloadedandaccessedlocallytheseservicesmakeitpossibletoaccomplish
complicatedtasksonlineandondedicatedhardware. WFAU’slistofVO serviceswillcontinuetogrowasnewIVOA standardsareimplementedandwiththeadditionofnewdatasetsliketheVISTA surveys.
GraphicInterfacestoExplanatoryAnalysisofAstronomicalImageDatabases
AvonHuxor (UniversityofBristol)with S. Phillipps
Inthisposterwewillpresentongoingworkinwhichearlydesignsforavisualinterfacetomassiveimagingdatabases, suchasSDSS,areoutlined. Althoughmanytoolsforthepresentationandanalysisofcataloguedataareavailable(e.g.TOPCAT),theserequirethattheimagedataisprocessedintointomoreabstract, typicallyquantitative, properties. Howeverintheexploratoryphaseofthescientificprocessthepropertiespresentinthecataloguesmaynotberelevant. Moreover, thelessonsfromCSCW(computer-supportedcollaborativeworking)showthatprematureformalisation(ShipmanandMarshall1994)mayhinderproductivity. Inearlierwork(Huxor1994), weshowedthevalueofamixedinterfacecombiningtheformalnotationofknowledge-baseswiththeinformalcomponentoffree-text. Weshowhowthisinterfacedesigncanbeextendedtoprovidesupportfortheexploratoryanalysisofastronomicalimagedatabases. Thisallowstheusetomanipulatetheformal'tags'associatewiththeimagesofobjectsofinterest,supportingbothformalandinformalreasoning.
Developingskillsfor“softwareastronomy”: aninnovativedistancelearningprojectforOpen
UniversitystudentsMarkJones (TheOpenUniversity)with
James Smith, and Alan Cayless
Theabilitytoaccesslargeastronomicaldatasetsremotelyandthedevelopmentofvirtuallearningenvironmentstogetherprovideaframeworkwhichpotentiallyallowsstudentstoconductastronomicalresearch. However, theexistenceofsuchsystems, initself, isnotsufficienttofacilitatetheeffectivedevelopmentofskillswhichwouldallowundergraduatestudentstomakeappropriateuseoftheavailabledata. HerewedescribeaprojecttoallowgeographicallyseparatedstudentstoworktogethertoformacompositequasarspectrumfromdatafromtheSloanDigitalSkySurvey. Drawingontheresultsofasmall-scalepilotstudy, wedescribethedesignanddevelopmentoftheteachingmaterialtosupportthisproject. Wediscusstheparticularchallengesposedindevelopingstudentsintheinformationhandlingandinformationliteracyskillswhicharerequiredtoconduct“databaseastronomy”.
SupportingDistributedScience: RunningGalaxyZoo
ChrisLintott (UniversityofOxford)withArfon Smith, and GalaxyZooteam
Sinceitslaunchin2007, GalaxyZoohasgrowntobetheworld'slargestastronomicalcollaboration,involvingmorethan250,000membersofthepublicinclassifyinggalaxies, simulatingmergersandhuntingforsupernovae. Developingandsupportingtheinfrastructurenecessaryforsuchalargeprojectbringschallengesofscalabilitythatmostmodernastronomyprojectsface. I willreviewthesolutiontheGalaxyZooteamhavefoundforsupportingsuchprojects(involvingextensiveuseofwebservicesandhostinginthecloud)alongwiththemethodsdevelopedtoturnrawclicksintoscience. Finally, I willconsiderthe
P10 55
impacttheavailabilityoflargenumbersofvolunteerswillhaveonfuturesurveysandprogramssuchastheLSST.
SoftwaretoolsforprocessingRHESSI visibilitiesAnnaMariaMassone (CNR-SPIN) with
Michele Piana
RHESSI imagingconceptistheoneofimagemodulation: theninepairsofrotatingRHESSIgridsprovideatemporalmodulationofthearrivingflux, whosepatternrepresentsaspecificsetofspatialFouriertransformofthesource. Thesecomplexdata, thepurestformoftheRHESSI datastream, arecalledvisibilities. ThistalkwillfirstdescribeanewsoftwaretoolforthecreationofregularizedelectronvisibilitiesassociatedtothephotonvisibilitiesmeasuredbyRHESSI.Thissoftwareprovidesthesolarphysicscommunitywithaneffectiveimagingspectroscopyprocedurewhereelectronmapsoftheflaringsourcearesynthesizedatdifferentelectronenergychannelsandasmoothingconstraintalongsuchenergiesisautomaticallyimposed. Thenaninterpolation/extrapolationimagingmethodwillbepresented, forthereconstructionofmapsfrombothphotonandelectronRHESSI visibilities.
ThehierarchicalstabilityofexoplanetarysystemsofBinarystarsusingtheCaledonianSymmetric
Four-Bodymodelwithanewglobalregularisationalgorithmtohandlecloseencounters
BonnieSteves (GlasgowCaledonianUniversity)with Anoop Sivasankaran, and Winston Sweatman
TheCaledonianSymmetricFourBodyProblem(CSFBP) (StevesandRoy, 2001; Szell, StevesandErdi, 2004: andShoaib, StevesandSzell, 2008)isarestrictedfourbodygravitationalmodelrelevanttothestudyofthestabilityandevolutionofsymmetricquadruplestellarclustersandexoplanetarysystemsoftwoplanetsorbitingabinarypairofstars. OneofthemaindifficultiesinstudyingtheCSFBP wasthefailingofthenumericalintegrationalgorithmtomaintainconservationofenergyandangularmomentumnearsingularitieswhichoccurredattwo-bodycloseencounters. RecentlywehavedevelopedaregularizationalgorithmtostudycloseencountersandcollisioneventsoccurringintheCSFBP(Sivasankaran, StevesandSweatman, 2009, 2010).
Inthisposterpaper, wewillillustratethat, thedevelopedregularizedalgorithmiscapableofhandlingthetwo-bodycloseencountersefficientlybyinvestigatingasetofCSFBP orbitscontainingcloseencounterevents. Theproposedregularisationalgorithmhasbetternumericalaccuracyandenergyconservingproperties. ItisnowpossibleforustoapplytheCSFBP modeltostudythestabilityandevolutionofsymmetricexo-planetarysystemsoftwoplanetsorbitingabinarystarsystem, includingthosesystemswhichpassthroughcloseencounters. WehavenumericallyverifiedthatthehierarchicalstabilityofthesystemdependsonananalyticalstabilityparametercalledtheSzebehelyconstant. TheSzebehelyconstantisafunctionofthetotalenergyandangularmomentumofthesystemanditdependsonlyontheinitialconditionsofthesystem. UsingthenewregularisationmethodforawiderangeofSzebehely'sconstantandinitialconditions, weareabletoverifythefour-bodyanalyticalstabilitycriterionofStevesandRoy(2001)andgiveanoverallstabilitycriterionforpairsofexo-planetsorbitingsymmetricbinarystarsystems.
P11Dodarkmatterhaloshavecusps?
ChrisBrook (JeremiahHorrocksInstitute, UCLan)
PureN-bodysimulationshaveshownthatcolddarkmatterhaloshavesteepinnerdensityprofiles,or"cusps". Yetobservationsofrotationcurvesofdiskgalaxiesinferaflatter, coredinnerdensityprofile. Usingselfconsistentcosmologicalgalaxyformationsimulations, weshowthattheinclusionofbaryons, whicharedynamicallysignificantintheinnerregionsofhalos, candramaticallyaltertheprofileofthedarkmatter. Oursimulationsresultin"bulgeless"diskgalaxieswithdarkmattercores.
Extremevaluestatistics: predictingthefrequencyofthedensestclustersandsparsestvoids
OlafDavis (Oxford)with Stephane Colombi,Julien Devriendt, and Joe Silk
Oneinterestingpropertyofrandomfields- suchastheobserveddensityfieldoftheuniverse- isthedistributionoftheirhighestmaximaandlowestminima. Inparticular, themaximaofthedarkmatterfieldtranslatetothethelocationsofthemostmassiveclusters, whichexistinthehighlynon-linearregimeofgravitationalclusteringandprobetheevolutionofthepowerspectrumundergravity.
TorelatethetheoreticalmaximaoftheDM densitywithobservedmaximainasmallregionoftheuniverserequiresanunderstandingofthebehaviourofsamplemaxima: thisisthedomainofextremevalueorGumbelstatistics.
Wepresentanalyticalcalculationswhichcanpredictthedistributionofsuchmaximaandminimafromtheunderlyingpowerspectrum, anddemonstrateagoodagreementwithsimulatedGaussianfields. WealsocompareourpredictionstotheHorizon4Πsimulation, acosmologicalscaledarkmattersimulationcontaining70billionparticles.
Potentialapplicationswillbediscussed, includinglikelihoodconstraintsonvoidcosmologies, andapplicationtoobservedCMB anomaliessuchasthecoldspotand'AxisofEvil'.
Probingthedarkmatterhalosofearly-typegalaxiesvialensing
IgnacioFerreras (UniversityCollegeLondon–MSSL)
Thecombinationofgravitationallensingongalaxyscalesandstellarpopulationsynthesisenablesustoconstrainthebaryonfractioningalaxies,probingtheinterplaybetweenthedarkmatterhaloandthebaryonphysicstransforminggasintostars.I willpresentrecentworkbasedonasampleofstrong(early-type)lensesfromtheCastlessurvey.Thecombinationofanon-parametricapproachtothelensingdataandtheanalysisoftheHST/NICMOS imagesofthelensgivearemarkablygoodagreementbetweenbaryonandlensingmassintheinnerregions. Theradialtrendofthebaryonfractionoutto4-5 Re isshown,alongwithitsconnectionwiththeFundamentalPlane. I willputthisresultincontextwithrecentestimatesoftheglobalbaryonfractioningalaxies.
Cosmologyonsmallscales: thestructureof(mostly)darkmatterhalos
CarlosFrenk (DurhamUniversity)
Thestandardmodelofcosmology- the"Λcolddarkmatter"model- isbasedontheideathatthedarkmatterisacollisionlesselementaryparticle,probablyasupersymmetricparticle. Thismodelhasbeenfamouslyverifiedbyobservationsofthecosmicmicrowavebackgroundradiationandthelarge-scaledistributionofgalaxies. However, themodelhasyettobetestedconclusivelyonthesmallscalesappropriatetomostastronomicalobjects, suchasgalaxiesandclusters. I willreviewourcurrentunderstandingofthedistributionofdarkmatteronsmallscaleswhichderiveslargelyfromlargecosmologicalN-bodysimulationsandIwilldiscussprospectsfordetectingdarkmatter,eitherthroughitsgravitationaleffectongalaxiesandclustersor, moredirectly, through γ−rayannihilationradiation.
SuddenFutureSingularitymodelsasanalternativetoDarkEnergy?
HodaGhodsi (UniversityofGlasgow)withMartinA. Hendry
Oneofthekeychallengesfacingcosmologiststodayisthenatureofthemysteriousdarkenergyintroducedinthestandardmodelofcosmologytoaccountforthecurrentacceleratingexpansionoftheuniverse. Inthisregard, manyothernon-standardcosmologieshavebeenproposedwhichwouldeliminatetheneedtoexplicitlyincludeanyformofdarkenergy. OnesuchmodelistheSuddenFutureSingularity(SFS) model, inwhichnoequationofstatelinkingtheenergydensityandthepressureintheuniverseisassumedtohold. Inthismodelitispossibletohaveablowupofthepressureoccurringinthenearfuturewhiletheenergydensitywouldremainunaffected. TheparticularevolutionofthescalefactoroftheUniverseinthismodelthatresultsinasingularbehaviourofthepressurealsoadmitsaccelerationinthecurrenteraasrequired. InthiscontributionIwillpresenttheresultsofthetestsofanexampleSFS modelagainstthecurrentdatafromhighredshiftsupernovae, baryonacousticoscillations(BAO) andthecosmicmicrowavebackground(CMBR).WeexplorethelimitsplacedontheSFSmodelparametersbythecurrentdatathroughemployinggrid-basedandMCMC searchmethods. ThisletsusdiscusstheviabilityoftheSFS modelinquestionasanalternativetothestandardconcordancecosmology.
LoCuSS:WeakLensingAnalysisof21GalaxyClustersatz=0.15-0.3
VictoriaHamilton-Morris (UniversityofBirmingham)with G.P. Smith, E. Egami, T. Targett,
C. Haines, and A. Sanderson
TheLocalClusterSubstructureSurvey(LoCuSS) isamulti-wavelengthsurveyof100X-rayluminousgalaxyclustersat0.15< z < 0.3, spanningX-raytoradiowavelengths. OneofthemainsciencegoalsistomeasurethesubstructureoftheDarkMatterdistributionwithinclustersandtocorrelateclustersubstructurewithresidualsonclustermass-observablescalingrelations. I willpresentadetailedstructuralanalysisof21clustersusingourHST/ACS SNAPSHOT data. Substructuresfoundinthe"non-parametric"lensingmassmapsarecomparedwithK-bandluminositymaps, andChandraX-rayfluxmaps. Thesethreeindependentprobesareincloseagreement, includingbothstructuresdetectedwithintheACS fieldsofview,and(inasub-setofclusters)structureslocated
56 P10–P11
outsidetheobservedACS fields. Usingthenear-IRdataasaprioronboththelocationandmassofsubstructureswithintheclusters, wethenuseaBayesianmethodbasedonLenstool(Julloetal.,2007), tofitmultipledarkmatterhaloestothesheardata. Ourobservationalresultsonthecomplexityoftheclustermassdistributionsarecomparedwiththeoreticalpredictionsofclustersubstructure.
TheZEPLIN-III DarkMatterSearchExperimentMarkusHorn (ImperialCollegeLondon)
TheZEPLIN-III experimentattheBoulbyUndergroundLaboratoryusesa12-kgtwo-phaseXenontimeprojectionchamberspecificallydesignedtosearchforDarkMatterWIMPs. Thedetectormeasuresbothscintillationandionisationsignalstodiscriminatebetweendifferentparticlespeciesinteractinginthedetector. ThisallowsnuclearrecoilsignaturesofWIMPstobeseparatedfromthemorenumerousbackgroundofeventsgeneratedbyphotonsandelectrons. Theresultsfromthefirstsciencerun, withapprox850kgdaysdataacquiredin2008, arepresented. Additionallythecurrentupgradeoftheexperimentwithnewultra-low-backgroundphotomultipliersandtheinstallationofaneutronvetoisshown. Theprospectiveoutcomeoftheforthcomingsecondsciencerunisthendiscussed.
A NewPixonWeakLensingClusterMassReconstructionMethod
DanielJohn (DurhamUniversity)with V.R. Eke,and L.F.A. Teodoro
Wepresentanewpixon-basedmethodforclustermassreconstructionsusingweakgravitationallensing. Pixonsareanadaptivesmoothingschemeforimagereconstruction, wherethelocalsmoothingscaleisdeterminedbythedata. Wealsointroduceanewgoodness-of-fitstatisticbasedontheautocorrelationoftheresidualsoftheshearfield. WetestouralgorithmonsimulatedlensingdatasetsusingNFW haloswithandwithoutsubstructure. WecompareourresultstopreviousmethodssuchasKaiser-Squires(KS), MaximumEntropy(ME) andtheIntrinsicCorrelationFunction(ICF ) andshowanincreasedaccuracyinthemassreconstructions. Wefinallydiscussfutureapplicationstodata.
WeighinggalaxiesusinggravitationallylensedSNLS supernovae
JakobJonsson (UniversityofOxford)withM. Sullivan, I. Hook, S. Basa, R. Carlberg,
A. Conley, D. Fouchez, D.A. Howell, K. Perrett,and C. Pritchet
Gravitationallensingbyforegroundmattercanmagnifyorde-magnifybackgroundsources.Standardcandles, liketypeIasupernovae(SNeIa),canthereforebeusedtoweightheforegroundgalaxiesviagravitationallensing. Wepresentconstraintsondarkmatterhalopropertiesobtainedusing175SNeIafromthefirst3-yearsoftheSupernovaLegacySurvey(SNLS).Thedarkmatterhaloofeachgalaxyintheforegroundismodelledasatruncatedsingularisothermalspherewithvelocitydispersionandtruncationradiusobeyingluminositydependentscalinglaws. Wecannotconstrainthetruncationradius, butthebest-fittingvelocitydispersionscalinglawagreeswellwithresultsfromgalaxy-galaxylensingmeasurements.ThenormalisationofthevelocitydispersionscalinglawsarefurthermoreconsistentwithempircalFaber-JacksonandTully-Fisherrelations.Wehavealsomeasuredthebrightnessscatterof
SNeIaduetogravitationallensing. ThisscattercontributesonlylittletotheSNLS sample(z < 1),butwouldcontributesignificantlyat z > 1.6.
Theimpactofdelensinggravitationalwavestandardsirensondeterminingcosmological
parametersCraigLawrie (UniversityofGlasgow)with
Martin Hendry, Fiona Speirits, and Joshua Logue
Recentlytherehasbeenmuchattentioninthecosmologyliteratureonthepotentialfutureuseofcompactbinaryinspirals, so-calledgravitationalwavestandardsirens, ashighprecisionprobesoftheluminositydistanceredshiftrelation.
Ithasbeenrecognised, however, thatweaklensingduetointerveninglargescalestructurewillsignificantlydegradetheprecisionofstandardsirens. Shapiroetal(2010)presentamethodfor"de-lensing"sirens, bycombininggravitationalwaveobservationswithmapsofcosmicshearandflexionalongeachsiren'slineofsight.
Inthispresentationweexploretheimpactofthisde-lensingprocedureforconstrainingcosmologicalparameters. UsingMonteCarlosimulationsweinvestigatetheaccuracywithwhichthedimensionlessdensityparametersmaybedetermined, beforeandafterde-lensing, withfuturedatafromtheproposedLISA satelliteandEinsteinTelescope.
DirectdetectionofdarkmatterPawelMajewski (RutherfordAppletonLaboratory)
DarkMatterisoneofthegreatestmysteriesinscience. Althoughitmakesuproughly25%oftheuniverse, ithasneverbeendirectlydetected. Forlastdecadesthehuntfordetectionofdarkmaterparticlehasacceleratedandbecameamotivationtomanyofingeniousexperimentsaroundtheworld. I willpresentreviewofexistingandplanneddarkmatterdirectdetectionexperimentswithfocusonthevarietyofimplementedexperimentaltechniques.
Theimpactofdarkmattercuspsandcoresonthesatellitegalaxypopulatio
JorgePenarrubia (UniversityofCambridge, IoA)with A. Benson, M. Walker, G. Gilmore,
A. McConnachie, and L. Mayer
InthistalkI willshowtheresultsfromN-bodysimulationsthatstudytheeffectsthatadivergent(i.e. "cuspy")darkmatter(DM) profileintroducesonthetidalevolutionofdwarfspheroidalgalaxies(dSphs). I willshowthattheresilienceofdSphstotidalstrippingisextremelysensitivetotheslopeoftheinnerhaloprofile. I willalsooutlinetheresultsfromcalculationsthatsimulatethehierarchicalbuild-upofspiralgalaxiesassumingdifferenthaloprofilesanddiscmasses, whichshowthatthesize-massrelationestablishedfromMilkyWay(MW)dwarfsstronglysupportsthepresenceofcuspsinthemajorityofthesesystems, ascoredmodelssystematicallyunderestimatethemassesoftheknownUltra-FaintdSphs. ThesemodelsalsoindicatethatamassiveM31discmayexplainwhymanyofitsdSphsfallbelowthesize-massrelationshipderivedfromMW dSphs. WealsouseourmodelstoconstrainthemassthresholdbelowwhichstarformationissuppressedinDM haloes,findingthatluminoussatellitesmustbeaccretedwithmassesabove 108--109Msol inordertoexplainthesize-massrelationobservedinMWdwarfs.
DarkMatterintheMilkyWayJustinRead (UniversityofLeicester)
Experimentsdesignedtodetectadarkmatterparticleinthelaboratoryneedtoknowtheverylocalphasespacedensityofdarkmatter, bothtomotivatedetectordesignandtointerpretanyfuturesignal. I discussrecentprogressonestimatingthisanditsimplications.
UnmodifiedGravityFergusSimpson (Edinburgh)with Brendan Jackson,
and John Peacock
Byrelaxingtheconventionalassumptionofapurelygravitationalinteractionbetweendarkmatteranddarkenergy, substantialalterationstothegrowthofcosmologicalstructurecanoccur.AsanillustrationI willexplorethecaseofexcessdarkmatterformingfromadecayingdarkenergycomponent. Simpleanalyticsolutionstothemodifiedgrowthratesarefoundforthesemodels.Furthermore, neglectingthesedarksectorinteractionscaninduceasignificantbiasintheinferredgrowthrate, potentiallyofferingafalsesignatureofmodifiedgravity.
Wave-mechanicsofLargeScaleStructureEdwardThomson (UniversityofGlasgow)with
MartinA. Hendry, and LuisF.A. Teodoro
SimulationsofLargeScaleStructureusingN-Bodycodeshavehelpeddefinethe Λ−CDM paradigm.WhileN-Bodycodesremainthemostpopularapproach, alesserknownmethodwasdevelopedintheearly90'sthatformulatestheequationsdescribinglargescalestructure(LSS) formationwithinawave-mechanicalframework. ThismethodcouplestheSchroedingerequationwiththePoissonequationofgravity. Thewavefunctionencapsulatesinformationaboutthedensityandvelocityfieldsasasinglecontinuousfieldwithcomplexvalues.
InthispresentationI willreviewsomeofthekeyfeaturesofthewave-mechanicalapproachtoLSS.Themethodavoidstheadditionofanartificialsmoothingparameter, asseeninN-bodycodes,andisabletofollow'hotstreams'- somethingthatisdifficulttodowithphasespacemethods. ThemethodiscompetitivewithN-bodycodesintermsofprocessingtime. Thewave-mechanicalapproachcanbeinterpretedintwoways: (1)asapurelyclassicalsystemthatincludesmorephysicsthanjustgravity, or(2)astherepresentationofadarkmatterfield, perhapsanAxionfield, wherethedeBrogliewavelengthoftheparticlesislarge.
EmpiricalConstraintsontheDarkMatterContentofDwarfSpheroidalGalaxies
MatthewWalker (InstituteofAstronomy,UniversityofCambridge)
Thedwarfspheroidal(dSph)galaxiesorbitingintheMilkyWay'shaloarethesmallest, faintestanddarkestknownobjectsforwhichinternalkinematicsimplyadarkmattercomponent. HereIdiscussconstraintsonthedensityprofilesofdSphdarkmatterhalosasderivedfromobservedstellarkinematics, andI assessthevalidityandeffectsofvariousmodelingassumptions. I considerrealisticobservationaluncertaintiesinthecontextofeffortstodetectdarkmatterindirectlyintheformofhigh-energyphotonsreleasedduringself-annihilationevents. I attempttoidentifythemostsuitabledSphtargetsforsuchsearches.
P11 57
P12TheFrequencyandCompositionofWater-Rich
ExtrasolarAsteroidsJayFarihi (UniversityofLeicester)with
M.A. Barstow, S. Redfield, P. Dufour, andN.C. Hambly
Theinterstellarmediumisnolongeraviablephysicalmodelfortheoriginofheavyelementsseenincoolwhitedwarfs. Instead, ongoingSpitzerandground-basedstudiesofalargenumberofsingle, metal-enrichedstarshavedemonstratedthesourceofthepollutionmustbecircumstellar. Wheredetected, thegeometryofthedustand(heavyelement)gasdisksorbitingcontaminatedwhitedwarfsareconsistentwithtidallydisruptedasteroidanalogs, ahypothesiswhichalsoaccountsforthevolatile-poor, rockycompositionofthephotosphericmetalsandcircumstellardebris. Tantalizingly, ahandfulofthesepollutedwhitedwarfsappeartocontainexcesshydrogen, anindicationthatthedestroyedminor(ormajor)planetcarriedinternalwater.
I willdescribetheevidenceforsuchwater-richextrasolarasteroids, andtheongoingworktoconfirmthishypothesisbysearchingforoxygeninexcessofthatexpectedfrommineraloxidesascommonlyfoundintheinnerSolarSystem. Theconfirmationofwaterinextrasolar, terrestrialplanetarybodieswillconstrainthefrequencyofenvironmentsfavorabletohabitableplanetformationandmayindicatethathabitatssuitabletoextremophilesarecommonintheGalaxy.
TheMain-BeltComets: Long-livedIceintheInnerSolarSystem
HenryHsieh (QueensUniversityBelfast)
Themain-beltcometsareanewly-identifiedclassofsmallbodiesinoursolarsystemwhichhavetheorbitsofmain-beltasteroidsbutexhibitcometaryactivityintheformofdusttailsorcomae,indicatingthepresenceofsublimatingice. Sincetheirdiscoveryin2006, theyhavedrawninterestduetotheunexpectedpresenceoficybodiesonstable(i.e. long-lived)innersolarsystemorbits,theirimplicationsforsolarsystemformation, andtheirastrobiologicalsignificanceasapossibleprimordialterrestrialwatersource. I willdetailtheadvancesmadeinthestudyoftheseunusualobjectssincetheirdiscovery, discussthemanyoutstandingquestionsthatstillremain, andconsidertheirroleinourunderstandingoftheoriginandpastandpresentdistributionofwaterinthesolarsystem.
NightsidePollutionofExoplanetTransitDepthsDavidKipping (Harvard-SmithsonianCenterfor
Astrophysics)with G. Tinetti
Hot-Jupiterexoplanetshavebeendiscoveredtoexhibitsignificantthermalemissionfromtheirdaysidebutefficientcirculationimpliessimilaremissionsignalsfromthenightsidetoo. Thisemissionactsasaself-blendandattenuatestransitdepths, particularlyatmid-infraredwavelengths.TheeffectisshowntocausechangesintheSpitzer-measuredtransitdepthsatthe1-σlevelforthecaseofHD 189733b. Weexplorehowthenightsidepollutioneffectalterstheinterpretationofexoplanetspectra, withemphasisonthesignatureofwater, andalsopresentmethodsforaccountingforthisattenuation.
TheDensitiesofKuiperBeltObjectsPedroLacerda (Queen'sUniversityBelfast)
ThecoldKuiperbeltobjects(KBOs)arebelievedtocontainasignificantfractionofvolatilesintheformofice. Thefewdensityestimatesthathavebeensecuredsupportthisidea. KBO bulkdensitiescanbeconstrainedinbinaries, ifthesize(albedo)known, orfromlightcurvedata(spinperiodandphotometricrange)undertheassumptionthattheobjectsarenearhydrostaticequilibrium. OneofthemajorsciencegoalsoftheHerschelkeyprogrammetostudyKBOswillbetomeasurethealbedosofroughly25binaryKBOsandestimatethesystemdensities. Tothisdate,mostoftheusefuldensityestimateshavecomefromlightcurveanalysis. I willoutlinewhatiscurrentlyknownaboutKBO densities, includingestimatesobtainedusingthemostrecentlightcurvedata. I willdiscusspossibletrendsbetweendensityandotherphysicalpropertiesandwhatthosemightbetellingusaboutthewatercontentandinteriorstructureofKBOs.
ObservationsandmodellingofwatervapourlinesintheHerschelSPIRE FTS spectrumoftheluminousred-supergiant, VY CanisMajoris
MikakoMatsuura (UniversityCollegeLondon)with JeremyA. Yates(UCL), MichaelJ. Barlow(UCL), Dugan Witherick(UCL), Roger Wesson
(UCL), E.T. Polehampton(RAL), BruceM. Swinyard(RAL),and HerschelMESS Keyprojectconsortium
Watervapouriscommonlyfoundintheatmospheresofoxygen-richredgiantsandsupergiants. TheHerschelSpaceObservatoryhascarriedoutaspectralsurveyofluminousM-supergiantVY CanisMajorisinthefar-infraredandsubmillimetre. Inparticular, the200-670micronregionhasbeenexploredforthefirsttimeusingtheSPIRE (SpectralandPhotometricImagingReceiver)FourierTransferSpectrometer(FTS).WepresenttheSPIRE FTS observations, togetherwithnon-localthermodynamicequilibriumSMMOLmodellingofthefar-infraredwater-vapourlines,dominantcoolantsintheoutflowsfromsuchstars.
AmasingWaterAnitaRichards (JBCA,UniversityofManchester)
Thewatermoleculeisoneofthefewknowntoproducenatural, cosmicmasers. Thesecanattainextaordinarybrightnesstemperatures(1017K)whichallowstheirpositionsandvelocitiestobemeasuredwithspatialandspectralresolutionsofmilli-arcsecandtensofm/s, usingradiointerferometerssuchase-MERLIN.Masersfromwater(anditsdaughter, thehydroxylradical)arefoundinenvironmentsfromcometstodiscsorbitingAGN.I willconcentrateontheuseofwatermaserstomeasurethekinematicsofmoleculargasandshocksinstar-formingregions.Lookingahead, ALMA willimagebothmaserandthermalwater(sub-)mmlines, potentiallyexcitingindicatorsofdifferentiationinproto-planetarydiscs.
CharacterisationofexoplanetaryatmospheresIngoWaldmann (UCL)
Amongthe400-plusexoplanetsdiscoveredtodate, anever-growingsampleofthetransitingvarietypresentthemselvesasgoodtargetsforfurthercharacterisation. Usingtransmission(whentheplaneteclipsesitshoststar)andemission(theday-sidethermalemissionoftheexoplanet)spectroscopyitispossibletostudytheatmospheric
compositionsoftheseso-called"hotJupiters"inmoreandmoredetail. ThefeasibilityofsuchmeasurementshasbeendemonstratedwithgreatsuccessusingSpitzerandHST intherecentyears.Mostnotablearethedetectionsofmolecularspeciessuchaswater, methane, carbonmonoxideanddioxideinthenearinfra-redforavarietyofplanets. Thesedetectionsallowustobuildupanintricatepictureoftheatmosphericcompositionsanddynamicspresent. AttheendoftheSpitzercold-phase, agapinspace-basedobservatoriesinthenear- tomid-infra-redhasemerged, callingforincreasedeffortsinground-basedtechniques.Withthedetectionofmethaneinfluorescence, intheL-band, onHD 189733b, ithasbeenshownthatsuchmeasurementsusingmedium-sizedtelescopesonthegroundarefeasible. Atthisconference, I willgiveanoverviewofwhathasbeendonefromthespaceandground, whatwehavelearnedfromtheseobservations, andhowtobuilduponourresultsinfuturedevelopments.
P13TheInfluenceofHotPlasmaPressureon
MagnetosphericStructureatSaturnNicholasAchilleos (UCL) with C.S. Arridge, and
P. Guio
AlthoughthegiantplanetsSaturnandJupiterbothhaverapidlyrotatingmagnetospheres, andplanetarydipolemomentsfarstrongerthantheEarth's, theydifferinseveralimportantaspects. Inthispresentation, weshowresultsofforcebalancecalculationsusingtheoreticalmagnetosphericmodelsforbothplanetswhichrevealthat: (1)TheplasmadiscinJupiter'soutermagnetospherehasastructureprimarilyduetoabalancebetweenhotplasmapressureandmagneticcurvatureforce;while(2)theanalogousregionatSaturnismaintained, inaddition, byamuchstrongerrelativecontributionfromcentrifugalforceassociatedwiththerotatingplasma. TherelativesizesofthiscentrifugalforceandthevariablehotplasmapressureatSaturnalsostronglyaffectthe'compressibility'ofthekronianmagnetosphere.
AlfvénWavesinPartially-IonisedandRecombiningPlasmas
EuanBennet (UniversityofGlasgow)withDeclanA. Diver, and LuisF.A. Teodoro
TheearliestexampleofapartiallyionisedcollisionalplasmawastheUniverseduringtheepochofrecombination, about380,000yearsaftertheBigBang. Thisisthefirsttimethatneutralspecies(atoms)weremade. Inthispaper, wemodelthepropagationofAlfvénwavesthroughthecosmicplasmaasitmakesthetransitionfromfullyionizedtoalmostneutral, aspartofawiderstudyoftheplasmaphysicsoftheepochofrecombination. Infact, thisworkshowsthatitisunlikelythatAlfvénwavescouldpropagatenormally, andsoarelimitedintheinformationtheycanconveyfromtheearlymagnetisedUniverse.
WepresenttheoreticalresultsandnumericalsimulationswhichshowthattransverseMHDAlfvénwavespropagatinginaplasmathatisundergoingsignificantrecombinationwillneithersurviveintheiroriginalform, norretaincharacteristicsrelatedtotheirinitialconditions.WefindthattheAlfvénwavesaresignificantlyaffectedbytherisingneutralgaspressure, coupled
58 P12–P13
withthefallingplasmapressure, whentheplasmaismomentum-coupledtotheneutralgas.
TheplasmavelocityfielddisturbanceoftheAlfvénwaveinducessoundwavesinthegaswhich(i)carryenergyaway, depletingtheAlfvénwaveenergy, and(ii)interactfurtherwiththeplasmatoinducemagneto-sonicwaves. Inthisway, thepropagationofAlfvénwavesisconsiderablychangedbytheevolvingionizationfraction. Theimplicationofthischangeinwavepropagationpropertiesliesmainlyinthemagneticdiagnostics:weshowthatthedetectedpolarizationofmagneticfieldarisingfromAlfvénwavespropagatingthroughrecombiningmatterissignificantlyperturbedcomparedtothenon-interactingcase.
TheShockingSizeofCometMcNaughtGeraintJones (UniversityCollegeLondon–MSSL)
with GeraintH. Jones, RobertJ. Forsyth, andAndre Balogh
InJanuary/Febuary2007, CometC/2006P1(McNaught)becamethebrightestcometfor40years. TheESA/NASA Ulyssesspacecraft, inanear-polarorbitabouttheSun, performedaserendipitouscrossingofMcNaught’siontail, withitsdeepestpenetrationofthetailoccurringonFebruary7(Neugebaueretal., ApJ 667, 1262,2007), atadistanceof ∼ 1.6 AU downstreamofthecomet’snucleus. Theadditionofionizedmaterialtothesolarwindthatoccursatproductivecometsleadstotheformationofabowwave/shock, asthesolarwindflowadjuststothepresenceofthecometaryobstacle. Here, wepresentourresultsofasearchforCometMcNaught’sbowshock, primarilyusingdatafromUlysses’smagnetometerinstrument, andcomparethemtothosederivedfromobservationsmadeduringtheUlyssestailcrossingofC/1996B2(Hyakutake)in1996, andthetargetedencountersofotherspacecraftwithcomets. Theresultsrevealthevastscalesoverwhichproductivecometscanaffecttheirsurroundings.
SearchingforEvidenceofStarSpotsinSTEREOHeliosphericImagerData
RobertKidd (LancasterUniversity)with J.A. Wild,C.J. Davis, and J.A. Davies
TheHeliosphericImager(HI) experimentsonboardNASA’sSTEREO satellitesaredesignedtoobservetheinterplanetaryspacebetweentheEarthandtheSuninordertoimagetransientsinthesolarwindsuchascoronalmassejections.However, alargenumberofstarsliewithinthebackgroundofeachimage, takingseveralweekstocrosstheimager’sfield-of-view. Assuch, HIdatacanpotentiallybeexploitedtostudychangesinthelightfromthesebackgroundstars. Starspots, likeSunspots, areareasofthestellarphotospherethatarecoolerthanthesurroundingregionsandthereforevisiblydarker. Asaspotmovesacrossthediskofastar, thereisacorrespondingdropintheobservedlightintensity;weseeksuchvariationsinSTEREO HI data. Inadditiontoobservationalfindings, basedupon3yearsofHI data, firstresultsfromasimplemodeltopredictlightcurvesforvariousstarspotdistributionswillbepresented. ThismodelwilldeterminethefeasibilityofdetectingstarspotsinHI dataandplaceconstraintsonsizesofspotsthatmightbedetectedinthisway. Ultimately, thestudyofspotsonstarssimilartoourSunwillindicatelevelsofstellaractivity, andbyextensiontheseverityofso-calledspaceweather, insolar
systemsoutsideourownandplacetheextremesoftheSun’svaryingactivityinawidercontext.
TheroleofH3+inplanetaryatmospheresSteveMiller (UCL) with Tom Stallard
Thesimplemolecularion, H3+, playsacrucialroleintracingenergyinputsintotheupperatmospheresofgiantplanets: itisthusatracerofmagnetospheric-ionosphericcoupling. Butitdoesmuchmorethanthat:
1)Itactsasasourceofionisation, playingapivotalroleinthegenerationofJouleheating; 2)Itgeneratesbothion- andthroughion-neutraldrag-neutralwinds, addingtotheenergybalanceoftheupperatmosphere; 3)Itactsasastabilisingcoolant- importantinthesolarsystemandbeyond.
Waytogoforsuchalittlemolecule!
Simplemodelsforclosedfieldlineregionsofthree-dimensionalrigidlyrotating
magnetospheresThomasNeukirch (UniversityofSt. Andrews)with
Nasser Al-Salti
Wepresentamethodtocalculatesimplethree-dimensionalsolutionsofthemagnetohydrostaticequationsintheco-rotatingframeofreferenceoutsidemagnetizedrigidlyrotatingcentralbodies,e.g. planetsorstars. Wemakenosymmetryassumptionforthemagneticfield, butneglectoutflowsandspecifyaparticularformforthecurrentdensity. Themagnetohydrostaticequationscanthenbereducedtoasinglelinearpartialdifferentialequationforapseudo-potential U ,fromwhichthemagneticfieldcanbecalculatedbydifferentiation. Theequationfor U canbesolvedbystandardmethods, insomecasesevenanalytically. Thesolutionscanalsobeusedtodeterminetheplasmapressure, densityandtemperatureasfunctionsofallthreespatialcoordinates. Despitetheobviouslimitationsofthisapproach, itcould, forexample, beusedasasimpletooltocreatethree-dimensionalmodelsfortheclosedfieldlineregionsofrotatingmagnetospheresofplanetsorstarswithoutassumingrotationalsymmetry.
LaboratoryExperimentstoinvestigatethemechanismsofAuroralKilometricRadiationKevinRonald (UniversityofStrathclyde)withD.C. Speirs, S.L. McConville, K.M. Gillespie,
A.D.R. Phelps, R. Bingham, A.W. Cross,C.G. Whyte, C.W. Robertson, W. He, R.A. Cairns,
I. Vorgul, and B.J. Kellett
ElectronsdescendingthroughtheauroralregionsoftheEarth’smagnetospherearesubjecttoanincreasingmagneticfield. Conservationofthemagneticmomentassociatedwiththeelectrontrajectoriesresultsintheelectronstreamformingahorseshoedistributioninvelocityspace. Intheregionsofdepletedplasmadensity(plasmafrequency << cyclotronfrequency)powerfulradiationemissionsareobservedintheX-modeclosetothecyclotronfrequency, ∼ 300kHz. Ithasbeenspeculatedthatthisradiationisassociatedwithrelaxationofthefreeenergyintheelectrondistributionbyakineticcyclotroninstability. Itisthoughtthatsimilarprocessesoccurinmanymagnetisedastrophysicalobjects.
Toprovidefurtherinsightintothisproblem, anexperiment(scaledtomicrowavefrequenciesbyincreasingthemagneticfield)hasbeendevisedattheUniversityofStrathclydewhereanelectronstreamisinjectedintoanincreasingmagneticfield
toformcomparableelectronvelocitydistributions.Theexperimentsareconductedinparallelwithanextensivenumericalsimulationprogramme, whichaidsinthedesignoftheapparatusandintheunderstandingoftheelectrodynamics. Theseexperimentsandsimulationshaveshownstrongagreementwithconversionefficiency(fromelectronkinetictowavefieldenergy)of∼ 1 − 3%, withtheemittedradiationneartotherelativisticcyclotronfrequency, propagatingandpolarisedperpendiculartothebiasmagneticfield.Theseresultsareconsistentwiththegeophysicalobservations.
Themostrecentmeasurementshaveintroducedabackgroundplasmaintothegenerationregion, tosimulatethedepletedbackgroundplasmaintheauroraldensitycavities. Onemayanticipatethatthisplasmawillbeclosetoupperhybridabsorptionresonancefortheradiationgeneratedbytheenergeticbeam. Thisplasmahasbeennotedtosignificantlyinhibittheradiationgenerationwhenthedensityexceedsacertaincriticallevel.
RadioobservationsofhighlyenergeticpulsarsPatrickWeltevrede (JodrellBankCentrefor
Astrophysics)
InthistalkI willcomparethecharacteristicsofradiopulsarswithhighandlowspin-downenergy-lossrates. Animportantconclusionisthatofthefractionallinearpolarizationintheradiobandisveryhighforhighlyenergeticpulsars. Thetransitionappearstohappenatthedeathlinepredictedforhigh-energycurvatureradiation,suggestingapossiblelinkbetweentheemissionphysicsofthe γ−raysandtheradio.
Itisarguedthatthemostdirectlinkbetweenthehigh-energyandradioemissioncanbefoundforthesubgroupofpulsarswhichwecalltheenergeticwidebeampulsars. Thesimilaritiesinpulsemorphologysuggestthatbothtypesofemissionareproducedatthesameextendedheightrangeinthemagnetosphereandpropagationeffectsinthemagnetospherecouldplayanimportantrole. Thelatterwouldnaturallyleadtodecouplingofthewavemodes, whichcouldexplaintheobservedhighdegreeoflinearpolarization.
Thereisgrowingevidencethatthebrakingtorqueofpulsarscausestheanglebetweenthemagneticaxisandtherotationaxistoevolveovertime. Thishasimportantconsequencesforevolutionarymodelsandforestimationsofthetotalnumberofneutronstars. Theunderlyingphysicsofthechangeinmagneticinclinationisfarfromunderstoodandthevalidityofthestandardformulatoderivequantitieslikethespin-downenergylossrateappeartobequestionable.
IonlosstotheSolarWindfromVenusatSolarMinimum
AlanWood (AberystwythUniversity)withS.E. Pryse, M. Grande, and ASPERA team
TheabsenceofanintrinsicmagneticfieldonVenusallowsthesolarwindtointeractdirectlywiththeionosphereandupperatmosphereoftheplanet. ThelossofionsfromtheVenusianenvironmenttothesolarwindhasdirectimplicationsfortheevolutionoftheplanetaryatmosphere. Escapemechanismsinducedbythesolarwindarethoughttobethedominantlossprocessesatsolarmaximumforheavyatmosphericgasessuchasoxygen.
P13 59
ObservationsconductedbyVenusExpressaroundsolarminimumwereusedtobuildmapsofionsofionosphericoriginwithintheVenusianenvironment. Theseobservationsshowedasymmetriesinboththedawn-duskandnoon-midnightplanes. Inthedawn-duskdirectiongreaternumbersofionswereobservedonthedusksidethanonthedawnside. Inthenoon-midnightplanegreaternumbersofionswereobservedonthedayside, althoughsignificantnumbersofionswereseennightwardoftheterminator. Collectivelytheseobservationssuggestedanightwardionflowdrivenbytheday-to-nightpressuregradient. Theionenergiessuggestedavelocityofseveralkm/s.
Theionmapsshowedthepresenceofoxygenionsuptoaltitudesoffewhundredsofkmonthedaysideandtoseveralplanetaryradiionthenightside. Inallsectorssomeobservationsshowedionswithenergiesgreaterthanthatrequiredtoescapefromtheplanet, withthelargestenergiesobservedintheshockedsolarwind. InviewoftheseobservationstwotypesofionlossmechanismsweresuggestedtooccuratVenusatsolarminimum. Atthehighestaltitudesplasmawaslostbydirectinteractionwiththesolarwind.Atloweraltitudesthenightwardflowacceleratedionsintothetailregionandsomeoftheseionshadsufficientenergytoreachtheescapevelocity.
P14TRACE/EUV observationofdrivenloop
oscillationsIstvanBallai (UniversityofSheffield)with
David Jess
InthisstudyweuseTRACE observationstocorroborateprevioustheoreticalwork, whichdeterminedtheresponseofacoronallooptoaharmonicdriverinthecontextofidealMHD,aswellasdeterminationofthemagneticfieldandthedegreeoflongitudinalinhomogeneity.WaveletandFouriertimeseriesanalysisareappliedtoTRACE imagesoftheperiodofinterest,andthephysicalparametersofthecoronallooparedeterminedusingseismologicaltechniques.Thestudiedcoronalloopisfoundtohavetwoperiodswhichcouldbeinterpretedasbelongingtothefundamentalandfirstharmonicbutalsocouldreflectthestageofanoverdrivenloop.Usingcoronalseismologicaltechniqueswedeterminethemagneticfieldinsidetheoscillatingcoronalloop. Theobtainedvaluesarefoundtobedependentonthescenarioemployedtoexplaintheperiodsofoscillations.
LongperiodoscillationsinsunspotsNickyChorley (UniversityofWarwick)withB. Hnat, V.M. Nakariakov, A.R. Inglis, and
I.A. Bakunina
Longperiodoscillationsofthegyroresonantemissionfromsunspotatmospheresarestudied.TimeseriesdatageneratedfromthesequencesofimagesobtainedbytheNobeyamaRadioheliographoperatingatafrequencyof17GHzforthreesunspotshavebeenanalysedandarefoundtocontainsignificantperiodsintherangeofseveraltensofminutes. Waveletanalysisshowsthattheseperiodsarepersistentthroughouttheobservationperiods. Thepresenceoftheoscillationsisconfirmedbyseveralmethods(periodogram, wavelets, Fisherrandomisationandempiricalmodedecomposition). Spatialanalysis
usingthetechniquesofperiod, power, correlationandtimelagmappingrevealsregionsofenhancedoscillatorypowerintheumbralregions. Alsoseenaretworegionsofcoherentoscillationofabout25pixelsinsize, thatoscillateinanti-phasewitheachother. Possibleinterpretationoftheobservedperiodicitiesisdiscussed, intermsoftheshallowsunspotmodelandtheleakageofthesolarg-modes. Wealsopresenttheanalysisoffollowingonesunspotoverthecourseof9days, showingthestabilityofthelongperiodoscillations, inboththebrightnesstemperatureandpolarisationdata.
BigBrightPoint, SmallBrightPoint, Cardboardbox
PhilipCrockett (Queen'sUniverstyBelfast)withMihalis Mathioudakis, David Jess, Sergiy Shelyag,
and Francis Keenan
PhotosphericMagneticBrightPoints(MBPs), arethesmallestmagneticfeaturesthatarecurrentlyresolvedonthesolarsurface. Beingomnipresent,highlymagneticobjects, MBPsmayprovidedetailsonthecreation, emergenceandevolutionofthesmall-scalekilogaussmagneticfield. High-resolutionG-bandimages, obtainedwiththerecentlycommissionedRapidOscillationsintheSolarAtmosphere(ROSA) instrument, weresubjecttoanewMBP detectionalgorithm. AdistributionofMBP areawasfoundtobeconsistentwithlognormalstatistics, peakingsubstantiallyabovethediffractionlimitedresolutionofthetelescope. A sharpdropofffromthepeaktothediffractionlimitindicatesalowerlimitinarea, belowwhichMBPstendnottoexist.
Flaresandglobalwaves, includingseismicHughHudson (SSL/UC Berkeley)with
C.A. Lindsey, and J.C. Martinez-Oliveros
Solarflaresarecloselyassociatedwithlarge-scalewavesorotherglobalsignaturesinthecorona(typeII bursts, EIT waves, andCMEs), Globalwavesalsoappearinthechromosphere(Moreton),andintheinterior("sunquakes"). Themorphologyofthesephenomenasuggeststhatallbeginincompactsourcesatlowaltitudesinthesolaratmosphere, andthattheirexcitationiscloselyrelatedtotheimpulsivephaseoftheassociatedflare. Forthecoronalandchromosphericsignatures, theeffectscannotnowbeobservedclosetotheirradiantpoints. Theseismicsignatureismostconspicuous15-60Mmawayfromthesource, and30-60minutesaftertheimpulsivephase. Wediscussthemorphologyandenergeticsoftheseglobaleffects. Weshowthatthemagneticrestructuringinvolvedinflareenergyreleaseultimatelymustexciteeachofthethem. Thisprocessmayinvolveintermediarystepsthatareinmostcasesnotwellunderstood.
ThelinkbetweenSodiumintensityenhancementsandthephotosphericmagneticfield
DavidJess (Queen'sUniversityBelfast)withMihalis Mathioudakis, Damian Christian,
Philip Crockett, Sergiy Shelyag, andFrancis Keenan
IntensityenhancementsintheSodiumD1absorptionlineat5896Angstromsareoftenusedasaproxyforstrongunderlyingmagneticfieldconcentrations. Utilizingarangeofhigh-resolutionimagersandspectro-polarimeters, weshowhowthiscorrelationbreaksdownatlowmagneticfieldstrengths. Furthermore, weapplymulti-wavelengthanalysistorevealhowSodiumbrightpointsarerelatedtotheirG-band
counterpartsthroughthedetectionofhigh-velocitydowndraftsonsmallspatialscales.
Longitudinaloscillationsinanexpandinghotcoronalloop.
MarialejandraLuna (UniversityofSheffield)withR. Erdélyi, and G. Verth
Wavesandoscillationscanprovidevitalinformationabouttheinternalstructureofthewaveguidetheypropagatein. Hereweinvestigateanalyticallythemagnetohydrodynamic(MHD)longitudinalwavesinanexpandingcoronalloop.ItisouraimtounderstandwhathappenstotheMHD waveswhentheyaregeneratedinafluxtubewherethefluxtubehasanon-constant(e.g.expandingormagneticbottle)geometry. Thegoverningequationofthelongitudinalmodeisderivedintheapproximationofweakexpansionandissolvedundersomefurtherbyanalyticalapproximations(e.g. inthelimitofthethinfluxtubeapproximation, spatialandtemporalscaling,etc.). ItisfoundthatthepropagationofslowlongitudinalwavesinanexpandingmagneticfluxtubecanbedescribedbytheKlein-Gordonequation. Solutionintheformofhypergeometricfunctionsisdeterminedforthelongitudinaloscillations. Therelevanceofthesesolutionsforsolarmagneto-seismologywillbediscussed.
ExploitingtheCoronalSlowModeMikeMarsh (JeremiahHorrocksInstitute, UCLan)
with R.W. Walsh
Observationsofthethree-dimensionalpropagationofwaveswithinactiveregioncoronalloopsandameasurementofthetruecoronalslowmodespeedareobtainedusingSTEREO.Intensityoscillationsareobservedtopropagateoutwardfromthebaseofaloopsystem, consistentwiththeslowmagnetoacousticmode. ThewavephasevelocityismeasuredintheobservationsfromtheA andBspacecraft. Thesestereoscopicobservationsareusedtoinferthethree-dimensionalvelocityvectorofthewavepropagationandmagnitudeof132±9km/s, givingthefirstmeasurementofthetruecoronallongitudinalslowmodespeed, andaninferredtemperatureof0.84±0.12MK.TheseresultsareconfirmedusingHINODEspectroscopicobservations. Itisfoundthattheloophasauniformtemperatureprofilewithameantemperatureof0.89±0.09MK,inagreementwiththetemperaturedeterminedseismologicallyusingtheSTEREO observations.Theresultsfurtherstrengthentheslowmodeinterpretation, andimplythatitisnotpossibletodiscriminatebetweentheslowmodephasespeedandthesoundspeedwithintheprecisionofthepresentobservations.
PropertiesofMHD wavesinplasmawithvariablebackground
RichardMorton (UniversityofSheffield)withR. Erdélyi
Thesolaratmosphericplasmaisanextremelydynamicmediumthreadedbyacomplexmagneticfieldthatisconstantlysubjecttoheatingandcoolingprocesses. Themagneticfieldprovidesthefoundationsforawidevarietyofplasmafinestructureinthesolaratmosphere, e.g.coronalloops, coronalholes, prominences. Eachofthesefeaturesinthesolaratmospherecansupportanarrayofmagneto-hydrodynamic(MHD)oscillatorymodes. WepresenthereafirststudyofthepropagationofMHD wavesinamagnetisedplasmaenvironmentthatiscoolingduetoradiation. Previousinvestigationshave
60 P14
concentratedontheaffectofradiationontheperturbationsonly. AnapproximateradiationfunctionthathastheformofNewtoniancoolingisusedforthesakeofsimplicity. WefindthatthecoolingoftheplasmaleadstoatimedependentfrequencyofMHD waves(oroscillations)andcausesbothdampingandamplificationoftheseperiodicphenomena. Thisresultcouldhaveimportantimplicationsforvariousaspectsofmagneto-seismologyinthesolaratmosphere.
PhasemixingintheSolarCoronaBeniaminOrza (TheUniversityofSheffield)with
I. Ballai, and A. Marcu
TheproblemofphasemixingofsolarAlfvénwavesisrevisitedtakingintoaccountdissipativephenomenaspecificforthesolarcorona.OurestimationsshowthatthepreviousresultsderivedincontextoftorsionalAlfvénwavephasemixingareheavilyunderestimatedsophasemixingcannotbeusedtoexplainthedampingoftorsionalAlfvénwavesandheatingofopencoronalstructures. Wealsoshowthatinorderforthephasemixingtostillbeaviablemechanismunrealisticassumptionshavetobemade.
CoupledAlfvénandKinkOscillationsinCoronalLoops
DavidPascoe (UniversityofStAndrews)withA.N. Wright, and I. DeMoortel
Observationshaverevealedubiquitoustransversevelocityperturbationwavespropagatingoutwardinthesolarcorona. ToinvestigatethenatureoftransversewavespropagatinginthesolarcoronaandtheirpotentialforuseasacoronaldiagnosticinMHD seismology, weperformthree-dimensionalnumericalsimulationsoffootpoint-driventransversewaves. Weconsidertheeffectofstructuringontheirpropagationandbehaviour.Whendensitystructuringispresent, resonantabsorptionininhomogeneouslayersleadstothecouplingofthekinkmodetotheAlfvénmode.ThedecayofthepropagatingkinkwaveasenergyistransferredtothelocalAlfvénmodeisingoodagreementwithamodifiedinterpretationoftheanalysisofRuderman&Robertsforstandingkinkmodes. NumericalsimulationssupportthemostgeneralinterpretationoftheobservedlooposcillationsasacouplingofthekinkandAlfvénmodes. Thiscouplingmayaccountfortheobservedpredominanceofoutwardwavepowerinlongercoronalloopssincetheobserveddampinglengthiscomparabletoourestimatebasedonanassumptionofresonantabsorptionasthedampingmechanism.
Theeffectofdensitystratificationonthetransverseoscillationsoftwoparallelcoronal
loopsDavidRobertson (SheffieldUniversity)with
M.S. Ruderman, and Y. Taroyan
Transverseoscillationsofcoronalmagneticloopsareroutinelyobservedduringthespacemissions.Sincethefirstobservationtheseoscillationswereinterpretedintermsofkinkoscillationsofmagnetictubes. Sometimescollectiveoscillationsoftwoormorecoronalloopsareobserved. Thismakesthedevelopmentofatheoryofcollectiveoscillationsofseveralloopsadesirableone.Anotherreasonforthedevelopmentofthistheoryisthatthereareevidencesthatatleastsomecoronalloopsarenotmonolithicbutconsistofmanythinmagneticthreads. Herethelineartheoryofkinkoscillationsoftwoparallelmagnetictubeswiththedensityvaryingalongthetubesis
developed. Thissystemisusedtostudytheeffectofdensityvariationontheeigenfrequenciesofcollectiveoscillations.
AnatomyofaslowwaveinacoronalloopTomVanDoorsselaere (UniversityofWarwick)
with Nick Wardle, GiulioDel Zanna, andKishan Jansari
Weanalyseanobservationofa5minutequasi-periodicoscillationdetectedinthecoronallineFeXII at195A,nearthefootpointofacoronalloopinHinode/EIS dataon08Feb2007. Thesameoscillationisdetectedsimultaneouslyintwoothercoronallines, FeXIII at204A andFeXI at192A.Theoscillationisobservedforafull2periodsinbothDopplershiftandintensity. WeuseFourierandwaveletanalysistodeterminetheperiodoftheoscillationtobeP =314±83sintheDopplershiftandP =344±61sintheintensity. WeobservenegligiblephaseshiftbetweenDopplerandintensitytimeseries. Thisisstrongevidencefortheinterpretationoftheobservedphenomenonintermsofapropagatingslowmagneto-acousticMHD mode. Forthefirsttime, weusespectroscopytodetectoscillationsintheelectrondensity, usingtheCHIANTI atomicdatabase.ComparingthedensityvariationsandtheDopplershiftsallowsustoderivetheline-of-sightcomponentofthephasespeed. Thecomparisonofthetemperatureandthedensityallowstoestimatethecoronalvalueoftheratioofspecificheats.
MagnetoseismologyofthechromospherewithtorsionalAlfvénwavesGaryVerth (KU Leuven)
InspiredbythefirstdiscoveryofsolarchromospherictorsionalAlfvénwavesbyJessetal. (2009), magnetohydrodynamictheoryisdevelopedwhichpredictshowtheobservableproperties, e.g., frequency, amplitudeandvelocity, areevolvingwhilepropagatingthroughrealisticallystratifiedchromosphericwaveguides.ItisfoundthatthesespecialincompressiblemagneticwavescanbefullyexploitedasauniquemagnetoseismologicaltooltoprobetheplasmastructureoftheSun'sloweratmosphere, e.g.,offeringarealandpracticalmappingofthe3-Dmagnetismofthesolarchromosphere. Theproposedtechniquescanbeappliedtothelatesthighspatial/temporaldatafromtheUK fundedROSA (RapidOscillationsintheSolarAtmosphere)instrumentorthemuch-awaitedSDO(SolarDynamicsObservatory)satellite.
Evidenceofmagneto-acousticwavesinphotosphericobservationsofasunspot
SergeiZharkov (UniversityCollegeLondon–MSSL) with S. Shelyag, R. Erdélyi, and
M.J. Thompson
WeshowtheobservationalevidenceforthepresenceofMHD wavesinthesolarphotospherededucedfromSOHO MDI andHinodeobservations. Themagneto-acousticoscillationsareobservedasacousticpowerenhancementinthesunspotumbraathighfrequencybandsinthevelocitycomponenttransversetothemagneticfield. Weusenumericalmodellingofthewavepropagationthroughlocalisednon-uniformmagneticfieldconcentrationalongwiththesamefilteringprocedureasappliedtotheobservationstoidentifytheobservedwaves. Underpinnedbytheresultsofthenumericalsimulationsweclassifytheobservedoscillationsasmagneto-acousticwavespropagatingalongthefieldlineswithAlfvenspeedandexcitedbythetrappedsub-
photosphericacousticwaves. Weconsiderthepotentialapplicationofthepresentedmethodasadiagnostictoolformagnetohelioseismology.
P15A near-infraredstudyoftheMagellanicSystem
withVISTA.GemmaBagheri (UniversityofHertfordshire)with
Maria-Rosa Cioni
TheMagellanicSystemrepresentsthenearesttemplatetostudystellarpopulationsandgalaxyinteractions. Itcomprisesoffourcomponents: theLargeMagellanicCloud(LMC),theSmallMagellanicCloud(SMC),theMagellanicBridge(MB) andtheMagellanicStream(MS).
RecentmeasurementsofthepropermotionoftheMagellanicClouds(Kallivayaliletal. 2006)suggestforthefirsttimethatthesegalaxiesareapproachingtheMilkyWay, supportingthetidalformationoftheBridgefromanLMC,SMCinteraction.
TheBridgeandtheStreamarewelltracedbythedistributionofneutralhydrogen, butthereareveryfewobservationsthatinvestigatetheirstellarcontent. IntheBridge, youngstarshavebeenfoundbyIrwin(1991), Grondinetal(1992)andothers, buttodatenostarshavebeenobservedinthestream.
Thisprojectwillusenear-infraredobservationsfromtheliteraturetoinvestigatetheformationandevolutionoftheMagellanicSystem'stidalfeaturesincludingacontributiontotheVMC strategyfortheBridge. TheunprecedentedsensitivityoftheVMC datashouldalsoallowforthefuturediscoveryofstarsintheStreamaspredictedbyMastropietro(2009), withdynamicalmodelsoftheMagellanicSystem.
TheVMC survey- I.StrategyandEarlyScienceData
Maria-RosaCioni (UniversityofHertfordshire)withVMC Team
ThefirstobservingseasonoftheVMC surveyhasbeencompleted. ThesurveystrategywillbebrieflydescribedtogetherandthefirstscienceresultsontheLargeMagellanicCloudwillbepresented.
TheVISTA ScienceArchiveRossCollins (IfA,Edinburgh)with R. Blake,
N. Cross, N. Hambly, M. Holliman, R.G. Mann,M. Read, E. Sutorius, and P. Williams
ThisyearmarksthestartofVISTA'ssurveyoperationsandallofthedatafromtheseinfraredobservationsoftheSouthernHemispherearearchivedbytheUniversityofEdinburgh'sWide-FieldAstronomyGroup. Databasereleasesofthesourcecataloguesandobservationmetadatawillbemaderegularlyandafteraproprietaryperiodbecomeavailablepublicly. Theseareaccessibleon-lineviaawebinterface(http://surveys.roe.ac.uk/vsa)aswellasthroughthestandardinternationalvirtualobservatoryinterfaces. Herewedemonstratehowuserscanmakebestuseofthearchivedatabasedesigntoquicklyextracthigh-qualityscientificresultsfromtheavailabledataset.
P14–P15 61
FindingvariablesusingtheVISTA ScienceArchiveNicholasCross (IfA,Edinburgh)with
Nigel Hambly, Ross Collins, Eckhard Sutorius,Mike Read, and Rob Blake
TheVISTA VariablesinViaLactea(VVV) willreobserve500squaredegressoftheGalacticPlaneandBulgeoverthenextfewyearsin ∼ 100
separateepochstofindperiodicvariablestars,whichwillbeusedasdistanceindicatorsofthestructureswithintheMilkyWay. Thiswillleadtoadatasetof1billionuniquesources(withupto100billionsingleepochdetections)ontheskyofwhichtheremaybe1millionvariables. TheVISTAScienceArchivemustbeabletorobustlyfindandcategorisevariablessuchthatscientistscaneasilyselectspecifictypes.
UltraVISTAJamesDunlop (UniversityofEdinburgh)withKarina Caputi, and UltraVISTA consortium
UltraVistaisanew5-yearultra-deepnear-infraredsurveybeingundertakenwiththeVistasurveytelescopeintheCOSMOS extragalacticfield. BythetimeofthismeetingwewillhavebeguntoreceivedatafollowingcommencementoftheVistasurveysinFeb2010. I willsummarizethedesignofthissurvey, andreviewitspotentialforthestudyofhigh-redshiftgalaxyevolutioninthelightofrecentresultsfromHST andSubaru. I alsoplantodiscusstheperformanceofVistafordeepimaginginthelightofourfirstdata.
VISTA PerformanceJimEmerson (QueenMary, UnivofLondon)with
Will Sutherland
VISTA commissioningwascompletedinthe3rdquarteranditwashandedovertoESO inDecember2010. Theas-builtperformancewillbecomparedtotherequiremnts.
HighredshiftquasarsintheVIKING field.JosephFindlay (QMUL)
Theexistenceofluminousquasarsatz ∼ 6
suggeststhattheformationofthefirstsuper-massiveblackholesbeganwithinthefirstfewhundredmillionyearsofthebigbang. Assuch,high-zquasarsofferpowerfulprobesoftheearlyuniverse, allowingconstraintsonearlystructureformation, chemicalenrichmentandthestateoftheintergalacticmediumattheendoftheepochofcosmicreionization.
Attheforefrontofhigh-zquasarsearchesinthenextdecadewillbetheVISTA Kilo-degreeINfraredGalaxysurvey(VIKING).VIKING beganitscoverageofthesouthernskyinNovemberandshouldhavetherightcombinationofareaanddepthtodetect ∼ 10z > 6.5 quasarsoverits1500sq.degfootprint. UsingthelatestobservationaldataI willdiscussthepotentialtodetectandisolate6.5 < z < 7.5 quasarsovertheVIKING field, makingparticularreferencetocolourselectionstrategies, samplecontamination,efficiencyandcompleteness.
FirstobservationsofstellarclustersintheLMCfromtheVMC survey
RoaldGuandalini (UniversityofHertfordshire)with VMC Team
WepresentfewpreliminaryresultsonananalysisweareperformingonthestellarclustersintheLargeMagellanicCloudobtainedthankstothefirstobservationsmadebyVISTA fortheVMC
survey. Webuiltupasampleofstellarclustersconsideringonlytheoneslocatedinoneofthetilesmostobservedinthefirstmonthsofthecampaign. Weshownear-IR color-magnitudeplotsforfewofthemand, finally, weremindwhatarethescientificgoalsthattheVMC surveycouldreachontheirstudy.
TheVISTA DeepExtragalacticObservations(VIDEO) Survey
MattJarvis (UniversityofHertfordshire)withDave Bonfield, and VIDEO Consortium
I willpresentthemainsciencegoalsoftheVIDEOsurveyandprovideanupdateonthestateofthedataandanyearlyscienceresults.
TheVISTA sciencepipelineJamesLewis (InstituteofAstronomy)with
Mike Irwin, Simon Hodgkin, Eduardo Gonzalez-Solares, and Peter Bunclark
TheVISTA telescope, withaninfraredcameracomprising162K×2K Raytheondetectorsanda1.7squaredegreefieldofview, representsahugeleapininfraredsurveycapabilityinthesouthernhemisphere. Pipelineprocessingofinfrareddataisfarmoretechnicallychallengingthanforopticaldata. Infrareddetectorsareinherentlymoreunstable, whiletheskyemissionisuptoa1000timesbrighterthanmanyobjectsofinterest, andvariesinacomplexspatialandtemporalmanner.Tocompensateforthis, exposuretimesarekeptshort, leadingtohighnightlydatarates. VISTA willgenerate ∼ 0.25TB pernightoverthenext5-10years, whichexceedsthetotaldatarateofall8mclassterrestrialtelescopes.
InthispresentationwediscussthesciencepipelinethathasbeendevelopedtodealwithimagingdatafromVISTA anddiscusstheprimaryissuesinvolvedinanend-to-endsystemcapableof: robustlyremovinginstrumentandnightskysignatures; monitoringdataqualityandsystemintegrity; providingastrometricandphotometriccalibration; andgeneratingphotonnoise-limitedimagesandscience-qualityastronomicalcatalogues.
VISTA VariablesintheViaLactea(VVV) andnewUKIDSS GPS highamplitudeIR variables
PhilipLucas (UniversityofHertfordshire)withD Minnitti, M Hempel, V Ivanov, M Rekjuba, and
R Saito
I describetheVVV synopticsurveyoftheGalacticBulgeandtheGLIMPSE-SouthregionoftheGalacticplanewithVISTA.Thissurveyhasrecentlybegunandnotmuchdataarereducedyet. However, I presentsomeearlyUKIDSS GPSresultsonnewintriguinghighamplitudevariablestarsfromtwoepochK bandphotometryofseveraldozensquaredegreesoftheplane,separatedby3years. A largeproportionofthenewvariablesarelocatedinasinglestarformationcomplex, SerpensOB2, suggestingthattheyarepre-mainsequenceeruptivevariableswithunsteadyaccretion, similartotherareclassofFUOrionisstars. I discussthepotentiallyveryseriousimplicationsforthestellarbirthlineandtheHRdiagramsinpre-mainsequenceclusters.
TheVISTA HemisphereSurveyRichardMcMahon (UniversityofCambridge)with
VHS collaboration
TheVISTA HemisphereSurvey(V HS) willresultincoverageofthewholesoutherncelestial
hemispheretoadepth4magnitudesfainterthan2MASS/DENIS inatleasttwowavebandsJ andK.IntheSouthGalacticCap, 5000squaredegreeswillbeimageddeeper, includingH band, andwillhavesupplementaldeepmulti-bandgrizY imagingdataprovidedbytheDarkEnergySurvey(DES).TheremainderofthehighgalacticlatitudeskywillbeimagedinYJHK andcombinedwithugrizwavebandsfromtheVST ATLAS survey, SDSSBOSS andSkymapper. Themediumtermscientificgoalsinclude: ahugeexpansioninourknowledgeof; thelowest-massandneareststars; decipheringthemergerhistoryourownGalaxy; measurementoflarge-scalestructureouttoz=1andmeasuringthepropertiesofDarkEnergy; discoveryofthefirstquasarswith z > 7
VariableStarsintheVISTA near-infraredY,J,KssurveyoftheMagellanicCloudSystem(VMC)
MariaIdaMoretti (BolognaUniversity)withGisella Clementini, Maria-Rosa Cioni,Vincenzo Ripepi, Marcella Marconi,
Massimo Dall'Ora, Jean-Baptiste Marquette, andVMC Team
VMC,theVISTA Y,J,KssurveyoftheMagellanicClouds(MCs)willprovidethemeanK-bandmagnitude(outof12epochtime-seriesdata)forMC pulsatingvariablesforwhichperiodsarealreadyavailablefromopticalmulti-epochsurveys(OGLE,MACHO,andEROS II).
ThefirstVMC datawerecollectedstartinginNovember2009andcoversixLargeMagellanicCloud(LMC) fields: theGAIA SouthernEclipticPolecalibrationfield; thefamous30Doradusregion; twofieldsintheproximityoftheBridgeconnectingthetwoCloudsandtwofieldintheLMC outerdisk.
CombininginformationsfromtheEROS-II(Tisserandetal. 2009, A&A,501, 985)andtheOGLE-III (Soszynskietal. 2009, ActaAstronomica, 59, 1)catalogues, wehavecompiledthelistofRR LyraestarsexpectedtofallintothesesixLMC fields. ThevisualdatacovertheR,B andV photometricbands, whiletheVMC datawillprovidetheY,J,andKsmagnitudes.
StartingfromthefieldthatGAIA willobserveintheLMC,wewilllookfortheVMC infraredcounterpartsofknownvariablestars, willconstructtheirK-bandlightcurvesandderivetheirmeanK-bandmagnitudesandpulsationparameters. WewillthenconstructPL relationsintheK-band. FromthescatteronthesePL wewillinvestigateeffectsduetometallicity, ageandotherstellarparameters. BysearchingfordistancevariationswewillproducethefirstsystematicinvestigationofthestructureoftheLMC.
VIKING,theVISTA Kilo-degreeInfraredGalaxySurvey
WillSutherland (QueenMary, UniversityofLondon)with VIKING Team
I willdescribetheVIKING surveywhichhasrecentlystartedobservationsonthenewVISTAtelescopeatParanal, Chile. Thesurveyaimstocover1500deg2 ofextragalacticsky, overlappingwith2dFGRS andSDSS.VIKING willsurvey5bands, Z,Y,J,H,Ks, toapprox1.5magdeeperthantheUKIDSS LAS.EarlyfieldsarebeingtargetedontheHerschel-ATLAS regions. I willdescribetheearlydataprocessingandqualitycontrol, andoutlinethesciencegoalsofthesurvey.
62 P15
P16TheOVRO OphiuchusPre-Stellar(OOPS) Survey:
A 3.4mmContinuumEmissionStudyofCircumstellarMaterial
JoannaBulger (UniversityofExeter)withJ. Patience, H. Arce, S. Corder, J Koda,
J. Carpenter, and A. Sargent
Circumstellardisksarethebirthsitesofplanetformation. Bothdiskmassanddustopacityspectralindexarecrucialdiskparametersinunderstandingtheearlystagesoftheplanetformationprocess. Millimetercontinuumemissionprobestheopticallythin, coolerouterregionsofcircumstellardisksandisthewavelengthrangeatwhichthebulkofthecircumstellarmaterialemits.Theresultspresentedareofa3.4mmcontinuumsurveyusingtheOVRO interferometer, onasampleof34membersoftheRhoOphiuchimolecularcloud, oneofthenearestsitesofongoingclusteredstarformation. ThesampleconsistsofbothstarlessclumpsandClass0-IIyoungstellarobjects(YSOs), spanningtheevolutionarysequenceoflowmassstarformation.Theseobservationsinvestigatecircumstellarmaterialintheformofacircumstellardiskandsurroundingenvelope. Continuumemissionisdetectedin22ofthesourcesata3σlevel(typically0.9mJy), withatypicalbeamsizeof3’’.7×2”.3.ThemeasuredfluxesofthebrightestClass0andfaintestClassII objectsare; 227mJyand3mJyrespectively. Thedustopacityspectralindex,indicativeofgraingrowth, ofthesesourceshasbeendeterminedfromthesefluxmeasurements,takenincombinationwithpreviousmillimeterwavelengthobservationsobtainedfromtheliterature. Estimationsofthetotaldiskmassesofthesesourceshavebeendirectlycalculatedfromthemeasuredfluxdensities. Finally, themolecularlineemissionsof; HCN(1 − 0) (88.62679GHz),HCO+(1-0)(89.18858GHz)andCO(1 − 0)
(115.2712GHz), wereobservedsimultaneouslywiththecontinuumemissionandthedetectionsofwhichareusedastracersofsystemoutflow.
HighResolutionRadioObservationsofIRASFSC10214
RogerDeane (Oxford)with Steve Rawlings,Ian Heywood, Hans-Rainer Klockner, and
Richard Saunders
Thegravitationallylensed, starburst/AGNcompositegalaxyIRAS FSC10214hasbeenthetopicof > 100 publicationsoverthepast19years. ObservationsacrosstheEM spectrumfromX-raytoradiowavelengthsrevealpuzzlingandsometimescontradictoryfeatures. WereportthehithertounexploredhighspatialresolutionpropertiesofthisenigmaticobjectthroughMERLIN observations. Furthermore, wepresentthespectralenergydistributionwhichincludesnewobservationsat330MHz(GMRT),15GHz(RyleTelescope)andpreviouslyunpublishedSpitzerphotometry. WecomparetheinfraredSEDwithanensembleofgalaxieswithsimilarpropertiesfromtheObreschkowetal(2009)semi-analyticsimulationtoinvestigatetheeffectsofdifferentiallensingoftheAGN andstarburstcomponents.
Thespatialdistributionofcoldgasinhierarchicalgalaxyformationmodels
HansikKim (DurhamUniversity)with C.M. Baugh,A.J. Benson, S. Cole, C.S. Frenk, C.G. Lacey,
C. Power, and M. Schneider
Thedistributionofcoldgasindarkmatterhaloesisdrivenbykeyprocessesingalaxyformation: gascooling, galaxymergers, starformationandreheatingofgasbysupernovae. Wecomparethepredictionsoffourdifferentgalaxyformationmodelsforthespatialdistributionofcoldgas. Wefindthatsatellitegalaxiesmakelittlecontributiontotheabundanceorclusteringstrengthofcoldgasselectedsamples, andarefarlessimportantthantheyareinopticallyselectedsamples. Thehalooccupationdistributionfunctionofpresent-daycentralgalaxieswithcoldgasmass> 109h−2M⊙ ispeakedaroundahalomassof∼ 1011h−1M⊙, ascalethatissetbytheAGNsuppressionofgascooling. ThemodelpredictionsfortheprojectedcorrelationfunctionareingoodagreementwithmeasurementsfromtheHI ParkesAll-SkySurvey. WecomparetheeffectivevolumeofpossiblesurveyswiththeSquareKilometreArraywiththoseexpectedforaredshiftsurveyinthenear-infrared. Futureredshiftsurveysusingneutralhydrogenemissionwillbecompetitivewiththemostambitiousspectroscopicsurveysplannedinthenear-infrared.
OriginoftheCosmicRadioBackgroundAndyLawrence (UniversityofEdinburgh)with
S. Singal, L. Stawarsz, and V. Petrosian
A cosmicradiobackgroundseveraltimeslargerthananticipatedhasrecentlybeendetectedbytheARCADE experiment. Wereviewpossiblesourcesofthisbackgroundincludingtrulydiffuseemission, lowsurfacebrightnessradiogalaxies,andradiosupernovae, butconcludethatthebestexplanationisaverylargepopulationofveryfaintradiosources. Thishassignificantimplicationsforoneormoreoftheearlyhistoryofstarformation,theearlygrowthofblackholes, andtheconfusionlimitforSKA.
Thee-MERGE LegacySurveyTomMuxlow (JodrellBankCentreforAstrophysics)
with Ian Smail, Ian McHardy, and e-MERGEconsortium
e-MERGE isanambitiousLegacysurveytoexploite-MERLIN'suniquecombinationofsensitivityandspatialresolutiontostudytheformationandevolutionofstar-forminggalaxiesandAGN outtoredshiftsof z > 5. Theseobservationswillprovideapowerful, obscuration-independenttoolformeasuringthemassivestarformationandAGNactivityinhigh-redshiftgalaxies, hencetracingthedevelopmentofthestellarpopulationsandtheblackholegrowthinthefirstmassivegalaxies.Witharesolutionof50-200masinC- andL-Bands, correspondingto < 0.5 − 1.5 kpcatz > 1, e-MERLIN givesusourfirsttrulyreliableviewofthedistributionofstar-formationwithintypicalgalaxiesattheepochwherethebulkofthestarsinthepresent-dayUniversewerebeingformed. e-MERLIN willdisentangletherelativecontributionsofAGN andstar-formation, anessentialstepgiventheapparentlysimultaneousgrowthoftheblackholesandstellarpopulationsingalaxies. e-MERGE willalsostatisticallycharacterizethenatureofthesub-uJyradiopopulationwhicharethetargetobjectsfortheSKA.
Theluminosity-dependenthigh-redshiftcut-offoftheradioluminosityfunction
EmmaRigby (IfA Edinburgh)with Philip Best,Mairi Brookes, Jim Dunlop, John Peacock,
Louise Ker, Huub Rottgering, and Jasper Wall
Weuseanewmodel-independentmethodtoinvestigatetheevolutionofthesteepspectrumradioluminosityfunctionandquantifythehigh-redshiftcutoff. TheanalysisusestheCENSORSradiosourcesamplethatwehavedevelopedoverthepastfewyears, combinedwithadditionalradiodatafromtheWall&Peacock, ParkesSelectedRegions, HerculesandVLA COSMOS samples.Wefindconclusiveevidenceforaluminosity-dependenthighredshiftcut-offinthesteepspectrumradiosourcepopulation. Thespacedensityoflowerluminositysources(P1.4GHz = 1025 to 1026 W/Hz)peakatorbelowredshiftone, withshallowdeclinestohigherredshifts, whilstathighpowersthecutoffmovestohigherredshifts(z > 2 for P > 1027 W/Hz)andbecomesmorepronounced. Theexistenceofahighredshiftcutoffisconfirmedwithhighstatisticalsignificance, andisrobusttoestimatedredshifterrorsandtovariationsintheradiospectralindexwithredshift. WediscusstheimplicationsoftheseresultsformodellingtheradiosourcepopulationthatwillbeobservedathighredshiftsbytheSKA anditsprecursors.
P17LaboratoryStudiesofNon-thermalDesorptionof
AcetonitrilefromIcyGrainMantlesAliAbdulgalil (Heriot-WattUniversity)with
Elizabeth Hall, Lars Finger, Lisa Hodgson, andMartin McCoustra
Formationofmoleculesintheinterstellarmediumisamajorquestionwhichattractsconsiderableattention. ItwasthoughtthatthesmallmolecularprogenitorstoEarthwereformedthroughthegasphasereactionsintheatmosphereofouryoungplanet. Morerecently, ithasbeenproposedthatnon-thermalreactionsininterstellarandcometaryicescanproducetheseprogenitorspecies[1].Acetonitrile(CH3CN) isonesuchmoleculethatmightbetheprecursoroflargerbiogenicmoleculessuchasaminoacids. Ithasbeenobservedinanumberofgalacticenvironmentssuchas: acoldmolecularcloud(L134N);protostellarices(NGC7538:IRS9), protostellarhotcoregas(SgrB2(N));andinacometarycoma(Hale-Bopp)[2]. CH3CN islikelyformedontheicygrainsviagas-grainreactionsbetweenCH3andCN radicals. CH3CN normallydesorbstothegas-phaseattemperaturesnear90K,howeverdesorptioncanbeinducedbylowenergyelectrons[3]. Thispaperwilldiscusstheadsorptionofacetonitrileonmodelinterstellardustsurfacesandtheeffectofelectronirradiationofsuchadsorbedspecies.
References
1- W.D.Geppert, E.V., M.Hamberg, V.Zhaunerchyk, M.Kaminska, R.D.Thomas, F.Osterdahl, F.Hellberg, A.Ehlerding, M.Danielsson, andM.Larsson. Proc. IAU Symp.,2008, 251, 349. 2- S.B.Charnley, S.D.R., Y.J.Kuan, andH.C.Huang, Adv. SpaceRes., 2002,30, 1419. 3- A.Belloche, R.T.G., H.S.P.Müller,K.M.Menten, C.Comito, andP.Schilke, Astron.astrophys, 2009, 499, 215.
P16–P17 63
Thedeuteriumchemistryinlowandhighmassstarformingregions
ZainabAwad (Dept. ofPhysicsandAstronomy,UCL) with Serena Viti, and Estelle Bayet
Observationsofdeuteriumininterstellarmediumhavelongbeenusedtoprobethephysicalconditionswithininterstellarclouds. Observationsrevealthatdeuteratedspeciesareabundantoverawiderangeofastrophysicalregionsincludingwarmandhotcoresaroundlow-massandmassivestars, respectively. Earlymodelsattempttostudydeuteriumchemistryandexplainthehighobservedfractionationviagas-phaseschemes. Itisnowconfirmedthatgrainsurfacereactionsplayaroleinformingmanydeuteratedspecies. Inthisworkwefocusontheimportanceofaddingdeuteratedspeciestochemicalnetworksusedinastrochemicalmodelsandanalysetheirinfluenceontheabundancesofdifferentspecies, inparticularinhotcoreregions. Theinfluenceofchangingtheenvironments'physicalconditionsontheabundancesofthespeciesisalsoconsidered.
Extragalacticstarformationactivity- propertiesoftheverydensegas
EstelleBayet (UCL) with S. Viti, D.A. Williams,J. Martin-Pintado, and S. Martin
Toincreaseourcomprehensionofthestarformationmechanismsingalaxies, itisessentialtofirstbetterdeterminethepropertiesofthegaswhichformsstars. Unfortunately, whenobservingextragalacticstar-formationregions, ionised,neutral, diffuse, molecularandverydensegasareallwellmixedinsidethebeam. Onlyatreatmentmixingtheoretical(astrochemistryandastrophysics)andobservationalapproachescanhelpdisentanglethegascomponentsandthusincreaseourknowledgeonthemechanismsinvolved. Inaddition, onecouldasks: howdoestheenvironment(e.g. nuclearactivity)influencethepropertiesofthedustandgas? MytalkwillaimatpresentingthelatestresultswehaveobtainedinUCL onthetwosubjectsdescribedabove.
InvestigatingtheOnsetofSilicateCrystallizationintheEarlyStagesofStarFormation
SeanChapman (UniversityofManchester)withCiska Kemper
SpectrafromtheShort-WavelengthSpectrometer(SWS) oftheInfraredSpaceObservatory(ISO)obtainedfordeeplyembeddedmassiveYSOswillbeanalyzedandcomparedtothoseinthediffuseISM toinvestigatetheonsetofcrystallizationofsilicatesinmassiveYSOs. FeaturescharacteristicofthecrystallinespeciesforsteriteandenstatitearecommmonlyseeninemissionindisksaroundclassI/II YSOs. HerewefocusonmassiveYSOs,intheearlystagesofstarformation(e.g. Class0).Theseobjectsexhibitsilicateabsorptionfeaturesinthemid-infrared, whichprobethecircumstellarenvironmentandthemolecularcloud. Silicateshavebeenfoundincircumstellardisksaroundyoungstarswithtypicalcrystallinitiesof10-20%,whilstnocrystallinecomponenthasbeenobservedinthediffuseISM.Wehopetoprobethefirststagesofcrystallizationofinterstellarsilicates,afterthesegrainshaveleftthediffuseISM andhavebeenincorporatedintostar-formingmolecularclouds.
IsotopicFractionationinPrimitiveMaterial:QuantifyingtheContributionofInterstellar
Chemistry.StevenCharnley (NASA GoddardSpaceFlight
Center)
AnomalouslyfractionatedisotopicmaterialisfoundinmanyprimitiveSolarSystemobjects,suchasmeteoritesandcomets. Itisthought, insomecases, totraceinterstellarmatterthatwasincorporatedintotheSolarNebulawithoutundergoingsignificantprocessing. Wewillpresenttheresultsofmodelsofthenitrogen, oxygen, andcarbonfractionationchemistryindensemolecularclouds, particularlyincoreswheresubstantialfreeze-outofmoleculesontodusthasoccurred.Therangeoffractionationratiosexpectedindifferentinterstellarmoleculeswillbediscussedandcomparedtotheratiosmeasuredinmolecularclouds, cometsandmeteoriticmaterial. Thesemodelsmakeseveralpredictionsthatcanbetestedinthenearfuturebymolecularlineobservations, particularlywithALMA.
ChemistryofdenseclumpsnearmovingHerbig-Haroobjects
HelenChristie (UniversityCollegeLondon)
LocalisedregionsofenhancedemissionfromHCO+, NH3andotherspeciesnearHerbigHaroobjects(HHO's)havebeeninterpretedasarisinginaphotochemistrystimulatedbytheHHOradiationonhighdensityquiescentclumpsinmolecularclouds. Staticmodelsofthisprocesshavebeensuccessfulinaccountingforthevarietyofmolecularspeciesarisinginthephotochemistry, butthetimescaleofthephotochemistrydevelopmentisrathershort, soithasbeendifficulttoreconcilethemodelswiththeobservednumbersofemissionregions. Thechemicalmodelhasbeenadaptedtoincludeamovingradiationsource. Thisallowssomephotochemically-inducedspecies, includingmethanol, tomaintainhighabundancesformuchlongerthanthepreviousmodels.
FirstResultsfromSHINING - SurveywithHerscheloftheISM inNearbyINfraredGalaxies
NatalieChristopher (UniversityofOxford)withE. Sturm, A. Contursi, R. Genzel, J. GraciaCarpio,
S. Hailey-Dunsheath, D. Lutz, A. Poglitsch,L. Tacconi, J. DeJong, J. Fischer, A. Sternberg,A. Verma, S. Madden, M. Sauvage, L. Vigroux,Diane Cormier, U. Klaas, M. Nielbock, H. Linz,J. Schreiber, O. Krause, D. Lemke, E. Schinnerer,
F. Walter, and M. Haas
OnbehalfoftheSHINING consortium, I willoutlinetheSHINING surveyandpresentsomeofthefirstresultsfromdatatakenduringHerschel'sScienceDemonstrationPhase.
SHINING isaHerschelguaranteedtimekeyprogrammeofthePACS consortium. Itisacoherentfar-infraredspectroscopicandphotometricsurveyoflocalandintermediateredshiftinfraredbrightgalaxies(starbursts, AGN,(U)LIRGs, andlowmetallicitygalaxies). AnimportantfractionofstarformationandAGNactivityintheuniversetakesplaceinsuchdusty,infraredbrightgalaxies.
Ourgoalistousethesuperiorsensitivity, spatialandspectralresolutionofHerscheltostudythesegalaxiesinawavelengthrangethatisleastaffectedbyextinction. Weaimtoobtainacomprehensiveviewofthephysicalprocessesatworkintheinterstellarmediumoflocalgalaxiesrangingfromobjectswithmoderatelyenhancedstarformation
tothemostdense, energetic, andobscuredenvironmentsinultra-luminousinfraredgalaxiesandaroundAGN.TheSHINING samplecoversawideparameterrangeinluminosity, activitylevel,andmetalenrichment, andwillbecomplementedbyafewobjectsatintermediateredshifts, i.e. atamoreactiveepochofstarformation.
TowardsUnderstandingtheFormationofWaterintheInterstellarMedium
VictoriaFrankland (Heriot-WattUniversity)withMarkP. Collings, and MartinR.S. McCoustra
Exposedtotheharshradiationfieldsofinterstellarspace, fewmoleculescanescapephotodestruction. However, thevastcloudsofgasanddustthataccumulateinthegulfsofspacebetweenthestars(knownastheinterstellarmedium)havebeenobservedtocontainmorethan120differentmolecularspecies[1]. Thelowtemperature(10-100K) andpressure(10−14
mbar)conditionswithintheinterstellarmediumlimittherangeofviablegas-phasereactionsresultinginthegas-phasechemistryalonebeinginsufficienttoexplaintheobservedabundancesofsomekeychemicalspecies(forexample, H2, andH2O).Dustgrainsprovideasurfaceonwhichadsorbedspeciescanreact[2]andhenceanalternativepathwaytokeyinterstellarmolecules.ThemoleculeofinteresthereisO2. TherecentODIN andSWAS campaignshavedeterminedthegaseousO2abundancetobeconsiderablylowerthanthatoftheatomicO abundance[3]implyingthatO2maybeadsorbedontothegrain.
SurfacechemistrywithinanultrahighvacuumchamberisbeingusedtoexplorethedesorptionkineticsofO2onarangeofastrophysicallyrelevantsurfaces. Intheseexperiments, theproductsareidentifiedusingtemperatureprogrammeddesorptionandinterpretedusingkineticanalysisofasimplesurfacemechanism.TheultimateaimofthisresearchwillbetocombineatomicbeamsofO andH tostudyinsituH2O formationonagrainsurface.
References
[1]from“129reportedinterstellarandcircumstellarmolecules”http://www.cv.nrao.edu/%7Eawootten/allmols.html(assessed11December2008)[2]R.GouldandE.Salpeter, Astrophys. J., 1963, 138, 393[3]K.Acharyya, G.W.Fuchs, H.J.Fraser, E.F.vanDishoeckandH.Linnartz, A&A,2007, 466, 1005
AstrochemistryintheALMA eraGaryFuller (JodrellBankCentreforAstrophysics-
UK ALMA ARC)
ALMA willrevolutionizethestudyofastrochemistryinboththisandothergalaxies. InthispresentationI willpresentrecentinitialresultsfromtheJCMT SpectralLegacySurveytogetherwithrecentresultsfromastrochemicalmodels.ThesewillbeusedtohighlighthowALMA willimpactourunderstandingofastrochemistry, and,consequentlystarformation.
ChemicalevolutioninNGC 6302(theButterflynebula)
KerryHebden (JodrellBankCenterforAstrophysics)with Gary Fuller
Observationsofthebutterflyplanetarynebula(PN)NGC6302revealacomplexbi-polarstructurewithamassivelow-velocitytoruscoupledwithhigh-velocityknots. Thismassiveexpandingtorushasahighmass-lossrate(∼ 1.5 × 10−4M⊙yr−1;
64 P17
Trungetal, 2008)andisbelievedtocontainthehighestmassofcircumstellarmaterialofanyknownPN (between ∼ 1 to3M⊙; Perettoetal,2007). ItsstrikingmorphologyalsoconcealsaperculiarchemistrywherebybothOH maserandPAH emissionhavebeendetected.
Shocks, x-raysandanencroachinghardradiationfieldpermeatingNGC 6302aresimilarpropertiestothosefoundinAGN andaccordinglyprovideanextremeenvironmentinwhichtotestmodelsoftheinteractionofUV photonsandx-rayswithmoleculargas.
WereporthereonthefirstdetectionofCN,HCN,HCO+andatentativedetectionofSiC2towardsNGC 6302madeusingtheJamesClerkMaxwellTelescope(JCMT).Thesemolecularspecies, alongwithCO,aremodelledwiththeMeudonPDRcodetoconstrainconditionsinthesource. Theeffectsof12C/13C chemistryonmolecularabundancesarealsomodelledtoascertaintheiraffectsontherichchemistryinNGC 6302.
HotcoremodelsatlowmetallicityNadyaKunawicz (JodrellBankCentrefor
Astrophysics)with Gary Fuller, Estelle Bayet,David Tideswell, Andrew Markwick, and
Tom Millar
Hotcoresarethoughttobetheprogenitorsofmassivestarformation. InthispresentationI willdiscussthemodellingoftheisothermalcollapseofadarkcloud, andthefollowinghotcorestage. Thehotcoremodelisatimedependentchemicalmodel, whichusestheUMIST databaserate06reactionnetwork. Threemodelshavebeencreated, torepresenttheGalaxy, theLargeMagellanicCloudandtheSmallMagellanicCloud. ThemodelsusechemicalabundancestakenfromobservationsofHII regionsintheirrespectivegalaxy. Themodeloutputshavebeenusedtopredictcolumndensities. TheseresultshavebeenusedwithRADEX topredicttheobservablefluxseenacrossahotcoreforvariousspeciesincludingCS,HCN,HNC andHCO+. Theeffectofdecreasingmetallicityonanobservablehotcoreisthereforebeingexamined. TheresultsfromthisprojectshouldbedirectlycomparablewithALMA observationsofhotcoresinothergalaxies.
Photon- andElectron-drivenProcessesinModelInterstellarIces
MartinMcCoustra (Heriot-WattUniversity)
Modernsurfacesciencetechniquesallowustoprobeinequisitedetailtheinteractionofphotonsandelectronswithmodelsoftheicymantlesexpectedtogrowondustgrainsinthedenseinterstellarmedium. Thistalkwilldiscusstheresultsofmeasurementsonasimplemodelicecomprisingbenzene(C6H6)adsorbedonwatericesurfaces. Photonexcitationataround250nmandelectronexcitationaround250eV willbediscussed. Theimpactofthesemeasurementsonourunderstandingofthenon-thermaldesorptionoficygrainmantleswillbeoutlined.
TheXgearProject- A NewEraforAstrochemicalModelling?
PaulRuffle (JodrellBankCentreforAstrophysics)with Andrew Markwick(JBCA), Helen Roberts
(QUB),and Tom Millar(QUB)
XgearstartedlifeasawrapperprogrammewritteninC thatcollectedparametersforrunningastrochemicalmodelsusingtheHMC (hot
molecularcore)FortrancodebySteveRodgers(1998), assubstantiallydevelopedandupdatedbyHelenRoberts(2002onwards), whichutilisesLSODE:theLivermoreSolverforOrdinaryDifferentialEquations(Hindmarsh1983;RadhakrishnanandHindmarsh1993). ThegoaloftheXgearProjectistoenableastrochemicalmodelstoberuneasilyandconsistently, withfullusercontroloverthemanyparametersthatmustbespecifiedtorunamodel. Theseparameterscanbedefinedonthecommandlineand/orinaplaintextconfigurationfile. However, inthelongertermweintendtobuildaPHP-MySQL front-endtoXgear, sothatmodelscanalsobesetupandrunusingaclientwebinterfacetoa(remote)Xgearapplicationserverorcluster. Theresultsfromrunningsetsofmodelscoveringvariouspartsofparameterspacecouldthenbestoredinadatabaseforsubsequentquerying. OtherenhancementscouldincludealternativemodelenginestoHMC andtheinclusionofadditionalprocessessuchasgas-graininteractions. Initially,chemicalreactionrateswillbetakenfromUDFA2006: thenewUMIST databaseforastrochemistry(Woodall, Agundez, Markwick-KemperandMillar2006), whichreplacedRate99: TheUMISTdatabaseforastrochemistry(LeTeuffetal. 2000).ThecodeforXgearwillbemadepubliclyavailableunderthetermsoftheGNU GeneralPublicLicense. WeexpectthecodetocompilesuccessfullyunderLinux, UnixandOS X,forboth32- and64-bitplatforms.
P18Magnetospheric-periodoscillationsinSaturn'sequatorialmagnetosphereandopentaillobes
throughouttheCassinimissionDavidAndrews (UniversityofLeicester)with
S.W.H. Cowley, L. Lamy, and G. Provan
Wepresentnewresultsofanalysisofthenear-planetaryperiodoscillationsinSaturn'smagneticfield, employingallavailableCassinidataobtainedtodate, includingduringtherecentSaturnequinox. Inthisanalysisweuseanewfittothepreviouslystudiedspatialvariationsinthephaseoftheseoscillations, anddeducesecularchangesintheirperiodicities. Pre-equinoxtheseequatorialmagneticfieldoscillationsarefoundtobeconsistentlyinphasewiththoseobservedonSouthern-hemisphereopenfieldlines, andhencewiththedominantcomponentoftheSaturnkilometricradiation(SKR) emission. Meanwhile,fieldoscillationsonopenfieldlinesintheplanet'sNorthernhemisphereareconsistentlyfoundtobeinphasewiththeweaker, longer-periodcomponentoftheSKR.Nearequinox, wehavenowobservedarapiddecreaseintheperiodoftheequatorialfieldoscillations. Consequencesofthesenewfindingsarediscussed.
InterpolationofexternalmagneticfieldsoverlargesparsearraysusingSphericalElementary
CurrentSystemsCiaranBeggan (BritishGeologicalSurvey)with
Sam McLay
Interpolationofthemagneticfielddisturbancestoapointremotefromanobservatorycanbeachievedbyemployingthelatitudinal-weightedarithmeticmeanofthefieldasmeasuredattwoobservatories, onetothenorthandonetothesouthofthepointofinterest. Analternativetechniqueforinterpolatingexternalmagneticfield
disturbancesacrosslargespatialareascanbeachievedwiththeSphericalElementaryCurrentSystem(SECS) methodusingdatafromground-basedmagneticobservatories. TheSECS methodrepresentscomplexelectricalcurrentsystemsasasimplesetofequivalentcurrentsplacedataspecificheightintheionosphere. Themagneticfieldrecordedatobservatoriescanbeusedtoinvertfortheelectricalcurrentsandsubsequentlyusedtointerpolateorextrapolatethemagneticfieldacrossalargearea. Weshowthatinvertingforinducedsubsurfacecurrentsystemsinadditiontoionosphericcurrentsystemscanresultinstrongimprovementstotheestimateofinterpolatedmagneticfield, particularlyintheradialcomponentofthefield. Wedemonstratethatrelativelyfewobservatoriesarerequiredtoproduceanestimatewhichisbetterthanthenullhypothesis(i.e. assumingnochangeinthefield)orinterpolationusinglatitudinalweightingofdatafromotherobservatories. WefurtherinvestigatetheapplicationoftheSECS methodinmid- tohighgeomagneticlatitudesusingaseriesofobservatorynetworkstotesthowwelltheexternalfieldcanbeinterpolatedoverlargedistances.
AnestimationoftheCarringtonflaremagnitudefromsolarflareeffects(sfe)inthegeomagnetic
recordsEllenClarke (BritishGeologicalSurvey)with
Craig Rodger(UniversityofOtago), Mark Clilverd(BAS), Thomas Humphries(BGS), Orsolya Baillie
(BGS),and andAlan Thomson(BGS)
InthisstudywereviewpreviousworktoestimatethemagnitudeoftheCarringtonsolarflare(1September1859)andre-examineobservationsofsolarflareeffects(sfe)ontheKewandGreenwichObservatorymagnetograms. A databaseofmorerecenteventsisconstructedfrom: existingsfedataavailableon-line; magneticobservatoryyearbooks; sfedatacollectedandprocessedbyEbroObservatory; additionalscalingofeventsusingone-minutevaluesfromvariousINTERMAGNET andWDC magneticobservatories; andGOES X-rayfluxdata. WeinvestigatefourofthelargesteventsindetailandalsothestatisticalrelationshipbetweensfemagnitudeandX-rayfluxwithrespecttosolarzenithangleandgeomagneticlatitudeandusetheresultstoestimatethesizeoftheCarringtonflare.
EstimatingtheExtremesinGeomagneticActivityAcrossEurope
EwanDawson (BritishGeologicalSurvey)withAlanP Thomson, and Sarah Reay
Rapidlychanginggeomagneticfieldvariationsconstituteanaturalhazard, forexampleinnavigationand, throughgeomagneticallyinducedcurrents, topowergridsandpipelinenetworks.Thecontinuousmagneticmeasurementsavailabletohelpusunderstandthishazardtypicallyextendbacklessthan100years; thisproblemofthelackofalong-termdatasetiscompoundedbythefactthatmuchoftheolderdataisalsoinanalogueform, orisonlyavailabledigitallyashourlyordailymagneticindicesormeanlevels. So, itmaynotyetbeclearwhatthetrueextremesingeomagneticvariationsare, particularlyatthetimescalesofsecondstominutesthatarerelevantforestimatingthehazardtotechnologicalsystems.
Wethereforepresentananalysisbasedontheapplicationofastatisticaltechnique- 'extremevaluetheory'- toanumberofdecadesofoneminutesamplesofmagneticdatafromobservatoriesacrossEurope, andexplore
P17–P18 65
estimatedmaximainfieldvariationsinthehorizontalstrengthanddeclinationofthefield.Thesemaximaareexpressedintermsofthegreatestmaximumthatmaybeobservedonceevery100and200years. Wealsoexaminetheextremesintheone-minuterateofchangeofthesefieldcomponentsonsimilartimescales.
Theresultsshouldfindapplicationinbothhazardassessmentandinnavigationapplications. Theresultscanalsobeusedtomorerigorouslyanswertheoften-askedquestion: "justhowlargecangeomagneticvariationsget?
SpritesandRelativisticElectronBeamsAboveThunderclouds
MartinFullekrug (UniversityofBath)withToby Whitley, and Michael Rycroft
Ithasrecentlybeendiscoveredthatparticularlyintenselightningdischargescangeneratespritesandsubsequentlyupward-directedrelativisticelectronbeamsabovethunderclouds. Thisextendsthephenomenonofrelativisticrunawaybreakdownbelievedtooccurinsidethundercloudstotheatmosphereabovethunderclouds. Thismarksaprofoundadvanceinourunderstandingoftheatmospherebecausewenowknowitactsasagiant, natural, particleaccelerator. TheacceleratedelectronscanreachsignificantrelativisticenergiesofsomeMeVduringtheirpassagefromthetroposphere, throughthemiddleatmosphere, intonear-Earthspace.Theserelativisticelectronbeamsconstituteacurrentabovethundercloudsandeffectivelytransferenergyfromthetropospheretothemiddleatmosphere. Thiscouplingprocesstherebyformsanovelelementoftheglobalatmosphericelectriccircuitwhichlinkstroposphericthundercloudstotheatmosphereabove.
SuperDARN observationsofthesub-auroralconvectionresponsetoenhancedgeomagnetic
activityAdrianGrocott (UniversityofLeicester)with
M. Lester, S.E. Milan, and T.K. Yeoman
A recentadditiontotheSuperDualAuroralRadarNetwork(SuperDARN),theBlackstoneradarislocatedat ∼ 50 degreesmagneticnorth, ∼ 10
degreesequatorwardofitsauroralcounterparts. Atthislatitudetheradarregularlymakesobservationsofplasmaconvectionequatorwardofthemainauroraloval. Theseobservationsreveallowvelocitysub-auroralionosphericscatterthatiswellcorrelatedwithboththeringcurrent(SYM-H)andauroralelectrojet(AE) indicesindicatingitisrespondingdirectlytogeomagneticactivity. Inthispaperwepresentsomestatisticalverificationofthisrelationship, andinvestigatethetimedelaybetweentheauroralenhancementsandthesub-auroralconvectionresponse. Inaddition, wepresentsomenear-conjugateTHEMIS observationsofamagnetosphericsubstormwhichsuggestadirectrelationshipbetweenlocalisedsubstormactivityandtheobservedsub-auroraldynamics.
ObservationsofGeomagneticStormsoveraSolarCycle: SomeInitialFindings
JamesHutchinson (UniversityofLeicester)withD.M. Wright, and S.E. Milan
Geomagneticstorms, periodsofintensesolarwind–magnetospherecouplingusuallyassociatedwithextremeconditionsinthesolarwindsuchascoronalmassejections(CMEs)orco-rotatinginteractionregions(CIRs), causelargeglobaldisturbancesintheEarth’smagnetosphere;
depositinglargeamountsofenergyintothemagnetotailandproducinganenhancedringcurrentandenergisingplasmatorelativisticlevels,throughyetunknownexcitationmechanisms.
ByexploitingdatafromtheAdvancedCompositionExplorer(ACE) spacecraftinconjunctionwithspace- andground-basedmeasurementsatEarthoverthelastsolarcycle, adatabaseofgeomagneticstormshasbeencompiledandanalysed. Herewepresentsomeinitialstatisticalfindingsfromasuperposedepochanalysisof157eventsidentifiedfromtheglobalSYM-H index. Diurnalvariationinstormactivityisobserved, alongwiththegeneraltrendofactivityoverthesolarcycle. RadarmeasurementsfromtheSuperDARN andauroralimagesfromthefar-ultraviolet(FUV) packageonboardtheIMAGEsatelliteandtheultravioletimager(UVI) onboardthePolarspacecraft, arealsopresentedusinganewradarbeamkeogramtechniquetodemonstratevariationsintheauroralovalduringstormconditions. Theresultsofcorrelationstudiesbetweenstormsizesandsolarwindinputthroughcommoncouplingfunctionswillalsobediscussed.
OverviewoflowenergyelectronobservationsinthevicinityofSaturn'smoonEnceladus
SheilaKanani (UniversityCollegeLondon–MSSL)with Geraint Jones, Gethyn Lewis, Chris Arridge,
Andrew Coates, and Dave Young
EnceladusresidesdeepwithinSaturn'smagnetosphere. Themagnetosphericplasmaincidentonthesatelliteisabsorbed, formingathermalplasmawakedownstreamofthemoon,andacavityinhigherenergypopulations. WhentheCassinispacecraftcrossesEnceladus'sL-shell,thesecavitiesareobservedasbriefdropoutsinenergeticparticlefluxes, ormicrosignatures, mostclearlyobservedbytheMagnetosphericImagingInstrument(MIMI).A surveyofthermalplasmaobservationsbytheCassiniPlasmaSpectrometer(CAPS) instrumenthasrevealedtheexistenceofvariousfeaturesinlowenergyelectronsclosetothetimesofmicrosignatures, orimmediatelybeforeoraftertheiroccurrence. Thesefeaturesvary; somepresentthemselvesasasetofdiscretespikes, coveringelectronenergiesof9-15eV andlasting, intermittently, uptotensofminutes. Othershowevidenceofinjectioneventsclosetothemoon'sorbitalplane. Wepresenttheresultsofasurveyoftheseperplexingfeatures, suggestpossiblecausesfortheiroccurrenceanddiscussresultsfromcloseEnceladusflybys.
NatureoftheringcurrentinSaturn’sdaysidemagnetosphere
StephanieKellett (UniversityofLeicester)withC.S. Arridge, E.J. Bunce, A.J. Coates,
S.W.H. Cowley, M.K. Dougherty, A.M. Persoon,N. Sergis, and R.J. Wilson
DeterminationofthephysicalnatureofSaturn'sringcurrent, i.e., theactualcombinationofcurrentsassociatedwiththeinertiaofthenear-corotatingplasmaandhotparticleeffects, hasbeenthesubjectofmuchdebateforalmost30years.
HereweinvestigatethenatureoftheringcurrentinSaturn’sdaysidemagnetosphereusingmagneticfield(MAG) andplasmaparticle(CAPS,MIMI andRPWS) datafromtwotypicalnear-equatorialpassesoftheCassinispacecraftspanningtheradialrangebetween ∼ 3 and ∼ 20RS (RS isSaturn'sequatorialradius, equalto60268km). Physically,
theplasmacurrentsthatformtheringcurrentareduetooneormoreofthreepossibleeffects; thespatialgradientoftheperpendicularplasmapressure, theanisotropyoftheplasmapressuresparallelandperpendiculartothefieldlines, andtheinertiaoftheflowing(near-corotating)plasma.WeexamineplasmaparametersobtainedbyCassiniforeachpassandcomparetheazimuthalcurrentdensityprofilesdeducedwiththoseobtainedfromcurrentdiskmodelingofthemagneticfieldperturbations.
WeshowthatthecurrentassociatedwiththePperp > Ppara pressureanisotropyofthewarmwatergroupionsisimportantinside ∼ 10RS ,cancellingasignificantfractionoftheotherwisedominantinertiacurrentinside ∼ 6RS . Theoveralltotalcurrentdensityprofileisthenfoundtobesimilartothatproducedbythepressuregradientcurrent, butaugmentedinstrengthbyfactorsof ∼ 1.5 − 2.0 bythedifferencebetweentheinertiaandanisotropycurrents. Thededucedcurrentdensityprofilesareingoodagreementwiththegrossfeaturesoftheprofilesdeducedfromcurrentdiskmodeling, thoughwiththecurrentdensitythenfallingmoresteeplywithradialdistancethanthe 1/r dependenceassumedinthemodel.
Towardsmodellingofhighlatitudemagneticfieldsfromsatellitedata
GemmaKelly (UniversityofLiverpool)withRichard Holme, and Alan Thomson
Recentlow-Earthorbitsatellitemissionshaveprovidedawealthofhighqualitydataallowingforimprovedmodelsofthenear-Earthgeomagneticfield. However, understandinginthehighlatituderegionsislaggingbehindduetothecomplexityoftheprocessesandinteractionsinthisregion. Weinvestigateresidualsbetweensomerecentmodels(CHAOS-2, T01andCM4)anddatafromtheCHAMP andØrstedsatellites, withtheaimofinvestigatinghowwellthemodelsfitthedata,particularlyregardingthehighlatituderegions.
Bylookingattheresidualsonanorbit-by-orbitbasiswehaveshownthatallthreemodelsshowverysimilarfeaturesintheresiduals. Wecanidentifycurrentsourcesthatareconsistentintimeandco-latitude, evenatveryquiettimes(Kp < 2o,night-sideonly). ThereisalsosomecorrelationbetweenthesizeoftheresidualsandlevelofactivityindicatedbythePC andAE indices. Wheninvestigatingtwo-dayaveragedresidualplotstheauroralovalcanbeidentified, andthereareenhancedresidualsoverthepolarcaps, forbothquietanddisturbedtimes. Thisinformationwillbefedintoamethodforimprovinggeomagneticfieldmodelsathighlatitudes.
CoordinatedgroundandspaceobservationsofGeospace: A viewfromthegroundMarkLester (UniversityofLeicester)
Thestudyofthesolarwindmagnetosphereionospheresystem, sometimesreferredtoasGeospace, isbestconductedbybringingtogetherarangeofobservationaltools. Specifically, itisimportanttounderstandthatbothinsitumeasurementsbyspacecraftandremotesensingofmeasurementsbyspacecraftandfromthegroundprovideanincomparabledatasetforsuchinvestigations. Inthelastdecadeorso, spacemissionssuchasCluster, ThemisandIMAGE,havebeenaugmentedbyarangeofgroundbasedsystems, suchascoherentandincoherentscatterradars, magnetometers, riometersandauroralcamerasandspectrographs. Herewepresentan
66 P18
overviewoftheimportanceofcoordinatedgroundandspaceobservationsinordertodevelopourunderstandingofthelargerGeospacesystem. Weillustratethiswithexampleswhicharetakenfromavarietyofinstrumentsandstudies, whichillustratethecomplexity, bothintimeandspace,ofthesystemwhichweareinvestigating. WealsonotetheopportunitiesthatexistforcontinuedexplorationofGeospacewiththecurrentandfuturemissionsandinstrumentsaswellasbythecombinationofdatasetsinnovelways.
GPS PlasmsphericimagingCathrynMitchell (UniversityofBath)with
P Spencer
ThispaperoutlinesamathematicalapproachtoimagingtheelectrondensitydistributioninthelowerplasmasphereusingGPS measurementsfromlowEarthorbit(LEO) satellites. Theproblemofionosphericimagingusingground-basedGPSmeasurementshasbeenstudiedforanumberofyears. Suchmethodshaveprovedextremelyusefulinprovidingdetailsofthelargerscalemorphologyoftheglobalionosphere. TheworkpresentedextendsthesemethodssoastobeabletoimagetheplasmasphereuptoaltitudesoftheGPSsatellitesat20000km. TheproblemoflimitedobservationsduetothesmallnumberofLEO’sinoperationisovercomebyconstrainingtheplasmasphericelectrondensitytobeconstantalongmagneticfieldlines. ItisshownthatacoordinatetransformfromasphericalcoordinatesystemtoonedefinedintermsofEulerpotentialsissufficienttoprovideunambiguoussolutions.PreliminaryresultsusingdatafromtheCOSMICsatelliteconstellationarepresentedshowingtheresponseoftheplasmaspheretochangesintheinterplanetarymedium.
TheresultsclearlyshowtheresponseoftheplasmaspheretochangesintheIMF magneticfieldareconsistentwithreportedobservationsfromotherauthorsusingindependentobservationtechniques. PotentialnewscientificinvestigationsintomajorstormswillbepossiblewhenGPS datafromtheforthcomingSWARM missionareavailableandtheseideasarediscussed.
Evidencefortheoccurrenceof 10.6hmagneticfieldoscillationsinSaturn’sequatorial
magnetosphereGabbyProvan (UniversityofLeicester)with
D.J. Andrews, S.W.H. Cowley, M.K. Dougherty,and L. Lamy
Andrewsetal. (2008)andProvanetal. (2009)reportedCassiniobservationsofnear-planetaryperiodmagneticfieldoscillationsinSaturn’snear-equatorialmagnetosphere, andshowedthattheirperiodwascloselysimilartotheslowly-varyingperiodof ∼ 10.8 hdeterminedbyKurthetal.(2008)frommodulationsofSKR radioemissions.Kurth. etal(2008)furtherreportedthattheseemissionsalsoexhibitedasecondperiodof∼ 10.6 h. FurtherinvestigationbyGurnettetal.(2009)revealedthatthe ∼ 10.6 hmodulatedemissionoriginatesfromtheNorthernhemisphere,whilstthe ∼ 10.8 hmodulatedemissionoriginatesfromtheSouthernhemisphere.Andrewsetal. (2008)andProvanetal. (2009)alsofoundsignificant‘jitter’inthephasesoftheequatorialoscillations, andpresentedevidencethatmuchofthisisnotduetomeasurementerrorsbuthasarealphysicalcause. Hereweshowthatthisphase‘jitter’isduetothesuperpositionintheequatorialmagnetosphereoffieldoscillationsattheSouthernperiodwithweakeroscillationsatthe
Northernperiod. Wedeterminetherelativeamplitudesoftheseoscillations, andthephaseoftheNorthernperiodoscillationsrelativetotheNorthernSKR modulation.
ObservationsandmodellingofartificialD-regionheatingseenbyARIES
AndrewSenior (LancasterUniversity)withM.J. Kosch, and F. Honary
ArtificialradiowaveheatingofelectronsintheD-regionisusedasadiagnostictechniqueforstudyingpolarmesosphericsummerechoes, aradarphenomenoncausedbyminuteiceparticlesinthevicinityofthemesopause. Recentstudiesoftheheatingusingthecross-modulationtechniquefoundthatmodelsusedtopredicttheheatingoverestimatedtheobservedcross-modulationbyafactorof1.5-2.5. TheAdvancedRio-ImagingExperimentinScandinavia(ARIES),ahigh-resolutionimagingriometersystem, observedchangesintheionosphericabsorptionofcosmicradionoiseduringD-regionheating. Theseobservationshavebeencomparedtopredictionsfromasimilarmodeltothatusedwhenanalysingthecross-modulationresults. Provisionalresultsshowthatthemodeloverestimatesthechangeincosmicnoiseabsorptionbyafactorofabout2.TheseresultsleadustoquestionthevalidityoftheusualmodelsofD-regionheatingbypowerfulHFradiowaves.
SCANDI:All-skyviewofmeso-scalespatialstructureinthethermosphereandion-neutral
couplingoverSvalbardTimothySpain (UCL) with A.L. Aruliah,H.-C.I. Yiu, I. McWhirter, E.M. Griffin,
A. Charalambous, M. Kosch, L. Baddeley,V.S.C. HowelI,and I. McCrea
TheUCL ScanningDopplerImager(SCANDI) isanall-skyFabry-PerotInterferometerthatislocatedattheKjellHenriksenObservatoryonSvalbardneartheEISCAT ESR radars. Itprovidesroutinenighttimeobservationsofthetwomostprominentauroralandairglowemissionsat630nmor557.7nm. Theseallowmeasurementsofthermosphericwinds, temperaturesandintensitiesataround240kmand120kmaltitude, whichroughlycorrespondtotheF- andE-regionionosphere. Itisoneof3existingSDIsintheworld; theothertwoaretheoriginalAlaskanSDIandMawson, AntarcticaSDI.RecentlythefirstconjugatestudyoftheupperthermospherewasmadebycomparingtheSCANDI withtheMawsonSDI.Theseinstrumentshaveupsetthestandardassumptionsofaslowlyvaryingthermosphere.EISCAT-SCANDI experimentsusinghightemporalandspatialresolutionmeasurementshaveshownlocalisedrapidresponsestoionosphericvariability(10sofminutesoverafewhundredkilometreshorizontaldistance), butalsoanunderlyinginertia.Theeffectsofthisbehaviourappearinunexpectedamountsofheatingandaccelerationoftheupperatmosphere, andhaveconsequencesforfeedbackmechanismsthroughtheneutralwinddynamo.
Observationsofdouble-peakedHF radarspectraduetomixedechoesfromnaturalandartificial
plasmairregularitiesHannahVickers (UniversityofLeicester)with
Terry Robinson
CUTLASS HF backscattertargetsmaybeartificiallyinducedthroughtheuseoftheEISCAT highpowerionosphericheatingfacilityatTromsø, NorthernNorway. Plasmairregularitiescreatedinthiswayareknowntobehighlyfield-alignedandusually
possesslowspectralwidth. Inthevicinityofnaturalwavesandirregularitiesundermoredisturbedgeophysicalconditionshowever, thespectralwidthofartificialirregularitiesasdeducedbythestandardSuperDARN ‘FITACF’analysis, canbesometimesappeartobebroadened. Inthiswork, wepresentsuchobservationsandemploytheBurgmaximumentropyanalysismethodtoCUTLASS HF radarspectra, combinedwithstandard‘FITACF’parametersandDMSP satellitemeasurementstoshowhowmixedartificialandnaturalHF echoesfromspatiallyseparatedsourcescangiverisetodouble-peakedspectraasaresultofdetectionattheedgesofantennamainlobe
Presentdaychallengesinunderstandingthegeomagnetichazardtonationalpowergrids
JimWild (LancasterUniversity)withA.W.P. Thomson, C.T. Gaunt, P. Cilliers,B. Opperman, L.-A. McKinnell, P. Kotze,
C.M. Ngwira, and S.I. Lotz
Solaractivitygivesrisetochangesinthenear-Earthspaceenvironment, oftenreferredtoasspaceweather, thatcanadverselyaffecttechnologiesonandabovethesurfaceoftheEarth. Forexample, theimpactofacoronalmassejectionontheEarth’sprotectivemagnetospherecanleadtoageomagneticstorm, boostingexistingmagnetosphericcurrents. ThesecurrentsystemscauselargemagneticvariationsthatinduceelectricfieldsinthesolidEarth. Thesefields, inturn, generategeomagneticallyinducedcurrentsthatflowinconductingpipesandwires, inwaysinfluencedbytheelectricalpropertiesofeachnetwork. Consequently, powergridsandpipelinenetworksatalllatitudesareatriskfromthenaturalhazardofGICs. Assolaractivitybeginstoincreasefromthedeepestsolarminimuminacentury, weconsiderthecurrentunderstandingofthishazard,asitaffectsmajorpowersystemsinEuropeandAfrica. Wealsosummarisewhatcanbesaidwithsomecertaintyaboutthehazardandwhatresearchisyetrequiredtoaddressoutstandingquestionsanddevelopusefultoolsforgeomagnetichazardmitigation.
TrackingsolarwindstructuresfromtheSunthroughtotheorbitofMars
AnthonyWilliams (UniversityofLeicester)withN.J.T. Edberg, S.E. Milan, M. Lester, and M. Franz
WithnodirectupstreammonitorsofthesolarwindateitherVenusorMars, thesolarwindinputstotheplasmaenvironmentsofbothplanetsmustbeinferred. Wepresentamethod, usingacombinationofimagesfromtheHeliosphericImagers(HI) ontheSolarTerrestrialRelationsObservatory(STEREO) andin-situmeasurementsfromtheAdvancedCompositionExplorer(ACE)situatedatEarth’sL1pointtotracktheprogressionofCorotatingInteractionRegionsthroughtheinnerheliosphere, andtopredicttheirarrivalatVenusandMars. Weshowtheresultsofthismethodforsolarminimumfrom1July2007to31July2008, demonstratingthatthereisgoodagreementbetweenexpectedarrivaltimesandobservedenhancedactivityateachplanet.
Comparisonsofplasmatransportinthehigh-latitudeionospheresoftheEarthandVenus.
AlanWood (AberystwythUniversity)withS.E. Pryse, M. Grande, and H.R. Middleton
ThepresenceofaplanetarymagneticfieldatEarthandtheabsenceofsuchafieldatVenusresultsinsubstantialdifferencesinthedynamicsandmorphologyofthehigh-latitudeionospheres. In
P18 67
bothcasesphotoionisationistheprimarymechanismbywhichthedaysideionosphereiscreatedwhileparticleprecipitationandtransportprocessesacttomaintaintheplasmadensitiesatnight. HoweverthemechanismsdrivingplasmatransportatEarthandVenusarefundamentallydifferent.
ResultsarepresentedfromtheterrestrialionosphereduringintervalswhentheIMF isnorthwardwhichshowthattheTongue-of-Ionisation(TOI) canbedrawnaroundtheperipheryofthepolarcap(Middletonetal., 2005)andintothenightsideionosphere(Woodetal.,2008). Inthemagneticmidnightsectorsubstormscanmodulatethehigh-latitudeconvectionpatternandhencealterthespatialdistributionoftheplasma(Woodetal., 2009). WhenthesolarterminatorislocatedinthemagneticmidnightsectorpolarcappatchescanformbythebreakupofaTOI duetovariationinthehigh-latitudeconvectionpatterndrivenbythechangesintheIMF (WoodandPryse, inpreparation). Plasmastructuresinthissectoralsoshowaclearseasonalvariationduetochangesinthethermospherewiththeratioofthepatchdensitytothatofthesurroundingionospherebeinggreaterinwinterthansummer(WoodandPryse, 2009).
AtVenusobservationsofionsathighlatitudesclosetothesolarterminatorshowasymmetriesinboththedawn-duskandnoon-midnightplanes.Theseresultsshow, forthefirsttime, thepresenceofanightwardionflowatsolarminimum. Thevelocityofthisflowincreaseswithaltitudeanditislikelytocontributetothelossofionsfromtheplanettothesolarwind(Woodetal., inpreparation).
CombiningincoherentscatterradardataandIRI2007tomonitortheopen-closedfieldline
boundaryduringsubstorms.EmmaWoodfield (LancasterUniversity)with
J.A. Wild, A. Senior, and A.J. Kavanagh
Thesizeofthepolarcap, andhencetheamountofopenmagneticfluxcontainedwithinit, isaveryimportantquantitywhenitcomestounderstandingthesubstormprocessaswellasreconnectionratesingeneral. Ground-basedproxiesoftheopen-closedfieldlineboundary(OCFLB) havethereforebeenofgreatinterestinrecentyears. InthisworkwebuildonpreviousstudiesbyAikioetal(e.g. Ann. Geophys., 24,1905-1917, 2006)whichuseacombinationofEISCAT electrontemperaturemeasurementsfromthemainlandandSvalbardtotrackthemotionoftheOCFLB.WedemonstratewhetherusingtheInternationalReferenceIonospheremodel(IRI2007)canenhancethismethodandmakeitapplicabletootherincoherentscatterradars. InparticularwemakeuseofEISCAT datatoinvestigatetheelectrontemperaturesignaturesoftheOCFLB duringalargenumberofsubstorms.
P19ImagingobservationsofX-rayalbedoina
compactdiskflareMarinaBattaglia (UniversityofGlasgow)with
Eduard Kontar, and Iain Hannah
X-raysfromsolarflaresourcesareanimportantdiagnostictoolforparticleaccelerationandtransportinthesolaratmosphere. However, theobservedfluxatEarthiscomposedofdirect
emissionandphotonswhichareComptonbackscatteredfromthephotosphere. Thiscontributioncanaccountforupto40%oftheobservedfluxatenergiesof30-50keV,evenforanisotropicsource. Wepresentimagingobservationsofacompactflareonthesolardisc.Thesourcefull-width-halfmaximumwasdeterminedatdifferentenergiesusingX-rayvisibilityforwardfitting. Theobservedsourcesizeincreasesanddecreaseswithenergywithamaximumsizeatabout40keV,contrarytoobservationsmadeinlimbevents. ThebehaviourisconsistentwithpredictionsfromMonteCarlosimulationsofX-rayphotontransportinwhichX-rayvisibilitieswerecomputedfromsimulatedmapsandfittedusingvisibilityforwardfit.
ParallelelectricfieldgenerationbyAlfvénwaveturbulence
NicolasBian (UniversityofGlasgow)withEduard Kontar, and John Brown
WeinvestigatethespectralstructureoftheparallelelectricfieldgeneratedbystronganisotropicAlfvénicturbulence, inrelationwiththeproblemofaccelerationandheatinginastrophysicalplasmas, includingflareselectrons. A low-β two-fluidMHD modelisusedtofollowtheturbulentcascaderesultingfromthenon-linearinteractionbetweenkineticAlfvénwaves, fromthelargeMHD scalesdowntothesmall"kinetic"scales.ScalingrelationsareobtainedforthemagnitudeoftheelectromagneticfluctuationsshowingtheturbulentelectricfielddevelopsacomponentparalleltothemagneticfieldatlargeMHD scales.Thespectrumoftheparallelelectricfieldcanbeeffectivelyusedtomodelstochasticaccelerationofelectronsduringsolarflares. Thequasi-linearmodelingoftheaccelerationprocessisdiscussed.
ParticleaccelerationattheSunPhilippaBrowning (JBCA,Universityof
Manchester)
Thisinvitedtalkwillgiveanoverviewofparticleaccelerationinsolarflares. Observationalaspectsofhighenergyparticlesinflareswillbebrieflysummarised. Themaintheoreticalmodelsofaccelerationonflareswillbeoutlined, focusingonmodelsofparticleaccelerationinreconnectingmagneticfields. Somechallengesforfutureworkwillbeproposed.
ParticleAccelerationinthePresenceofWeakTurbulenceatanX-TypeNeutralPoint
ChristinaBurge (UniversityofGlasgow)withAlec MacKinnon, and Panagiota Petkaki
Itiswellknownthatparticlesinspaceplasmascanbeenergisedbyinteractionwithreconnectionregions, whichformatmagnetictopologicalfeaturessuchasnullsandseparatrices.Suchenergisationhasbeenstudiedinsimple, large-scalefields. Hereweextendthesestudiestoincludenoisy, turbulentelectricandmagneticfields.Themagneticfieldisperturbedbyasuperpositionofcoldplasmaeigenmodes,includingself-consistentelectricfieldoscillations,constructedasintheworkofCraigandMcClymont. Weakturbulenceismodelledbyadoptingrandomphasesfortheseeigenmodes.Usinganadaptivestepsizemethodwenumericallyintegrateparticleorbitsinrealisationsofthisfieldanddescribetheresultingparticledistributions.
Roleoflatitudeofsourceregioninsolarenergeticparticleevents
SilviaDalla (JeremiahHorrocksInstitute, UCLan)with Neus Agueda(UC Berkeley)
MeasurementsofSolarEnergeticParticles(SEPs)ininterplanetaryspacecanbeusedtoconstrainmodelsoftheiraccelerationduringeruptiveeventsattheSun, providedthattherolesofmagneticconnectiontothesourceandofinterplanetarytransportareunderstood. ItiswellknownthatthelongitudeofthesourceregionattheSunisakeyparameterindeterminingwhetheranSEP eventwillbedetectedanditscharacteristics.
HerewediscusshowthelatitudinalseparationbetweensourceregionanddetectingspacecraftinfluencestheprobabilityofobservingSEPsat1AU.Weselectasampleof477solarflaresofmagnitudegreaterthanC8.0, locatedinthewell-connectedlongitudinalrangebetweenW20andW80, andanalysewhetherornotanassociatedSEP eventisdetectednear-Earth. WeconsiderprotonmeasurementsbyGOES andelectrononesbyWIND/3DP.
Theseparationinheliolatitudebetweeneachflareregionanddetectingspacecraft, D,variesbetween0and30degreesinthissample. WefindanincreasedprobabilityofSEP detectionforDbetween4and12degrees. ValuesofD below4degreesandbetween12and28degreesarecharacterisedbyanSEP probabilityabouthalfthatinthe4-12degreerange.
MeasurementofAnisotropyinSolarFlareElectronSpectrausingRHESSI HardX-Ray
Spectroscopy.EwanDickson (UniversityofGlasgow)with
Eduard Kontar
Theangulardistributionofelectronsacceleratedinsolarflaresisakeyparameterinunderstandingtheaccelerationandpropagationmechanismsthatoccurthere. Howeverthisanisotropyisstillapoorlyknownquantitywithobservationalstudiesproducingevidenceforanisotropicdistributionandtheoreticalmodelsmainlyconsideringthestronglybeamedcase. Theeffectofphotosphericalbedocanbeusedtoinferthisanisotropyasitinfluencesdifferentlydirectedphotonsallowingdiagnosticsoftheangulardistributionintheelectrondistribution. A bi-directionalapproximationwasappliedandaregularizedinversionwasperformedonHardX-rayobservationsmadebyRHESSI inordertodeducetheelectronspectrainbothdownward(towardsthephotosphere)andupward(awayformthephotosphere)directions. Todetermineiftheanisotropychangessignificantlyovershortperiodsoftime. Intervalslasting4, 8and16seconds, overtheimpulsivepeakoftheflarewereexaminedforanychangeinanisotropy. ThiswasappliedtofoursuitableflaresdetectedbyRHESSI.Thedistributionsdeterminedwereconsistentwiththeisotropiccase.
Particleaccelerationinafragmentingcurrentsheet
MykolaGordovskyy (UniversityofManchester)with P.K. Browning, and G.E. Vekstein
Protonandelectronaccelerationisinvestigatedbasedontheforcedreconnectionmodelinwhichtheinitialcurrentsheetfragmentsintoaseriesoflocalisedcurrentfilamentsandmagneticislands.WeusecombinationofMHD andtest-particleapproachestoconsiderparticletrajectoriesconsistentlywithatime-dependentreconnection
68 P18–P19
model. Itisshownthatacceleratedparticlesinsuchamodelformtwodistinctivepopulations.ProtonsandelectronsmovinginopenmagneticfieldhaveenergyspectrawhichareacombinationoftheinitialMaxwelliandistributionandapower-lawhigh-energy(> 10keV) tail. Thesecondpopulationcontainsparticlesmovinginclosedmagneticfieldaroundo-points. Theseparticlesmovepredominantlyalongtheguidingfieldandtheirenergiesfallwithinquiteanarrowrangebetween100keV and10MeV.Itwasalsofoundthatparticlesmovinginclosedmagneticfieldhaveconsiderablyhigherpitch-anglesthanthosemovingintheopenconfiguration.
ParticleMotionandEnergyGainsinKinematicMHD modelsofCollapsingMagneticTrapsKeithGrady (UniversityofStAndrews)with
Keith Grady, and Thomas Neukirch
Duringsolarflaresalargenumberofchargedparticlesareacceleratedtohighenergies, buttheexactmechanismresponsibleforthisisstillunclear. Accelerationincollapsingmagnetictrapsisoneofthemechanismsproposed. WediscussanalyticidealkinematicMHD modelsforcollapsingmagnetictraps. Particleorbitsarecalculatedusingtheguidingcentreapproximation. Anillustrativeexampleofacollapsingmagnetictrapmodelwillbepresentedtogetherwithsomestudiesoftheeffectsoftheinitialconditionsoftheparticlesonthetrappingtimesandparticleenergygains.
Temporal, Spectral, andSpatialAnalysesofX-rayEmissionComponentsinImpulsiveSolarFlares
JingnanGuo (UniversityofGlasgow)withSiming Liu, Lyndsay Fletcher, and Eduard Kontar
Plasmaheatingandparticleaccelerationarethekeyissuesinsolarflarestudy. TwodistinctX-rayemissioncomponentsareoftenidentifiedinsolarflare. Theimpulsive, non-thermalhardX-raycomponentnormallyoriginatesfromthechromosphericfootpoints, whilethemoregradualthermalandsoftX-rayemissionoftenoriginatesfromcoronalsources. UsingRHESSI X-raydatawecalculatethetime-derivativeofsolarflarephotonlightcurvesindifferentenergybands. Theenergydependenceofthefluxchangerateanditstimeevolutionisstudiedforawellobservedsolarflare.A lower(higher)rateisexpectedforthelower(higher)energycomponent, andthetransitionenergybetweenthelowandhighratecomponentswillbecomparedwiththetransitionenergybetweenthethermalandnonthermalcomponents.Thisstudywillhelpusquantitativelyunderstandtherelationbetweenenergeticnon-thermalelectronsandhotplasmasresponsiblefortheobservedsoftX-rays. ThisworkissupportedbytheEU'sSOLAIRE ResearchandTrainingNetworkattheUniversityofGlasgow(MTRN-CT-2006-035484).
Cantheinfluenceofturbulentdensityperturbationsinthecoronabedetectedinflare
X-rayspectrum?IainHannah (UniversityofGlasgow)with
E.P. Kontar, and H.A.S. Reid
RHESSI solarflarehardX-rayobservationssometimescannotbeadequatelyinterpretedintermsofpurelycollisionalelectrontransport. Weinsteadpresentnumericalsimulationswhereweconsidertheenergeticelectron-beaminteractionsinthepresenceoflowfrequencydensityperturbations. Wedemonstratehowtheturbulentdensityperturbationsaffectthehighfrequency
Langmuirwavesandinturn, theflareacceleratedelectrondistribution. Theconsequencesofthisself-consistenttreatmentarediscussedfortheobservableX-rayspectrum.
CoronalmagnetictopologyandthesolarsourceofmajorSEP events
ChuanLi (UniversityCollegeLondon–MSSL) withC.J. Owen, S.A. Matthews, Y. Dai, and Y.H. Tang
A statisticalsurveyofthemajorelectroneventsduringtheperiod2002Februarythroughtheendofsolarcycle23ispresented. Wehaveobtainedelectronreleasetimesandthepeakfluxspectra.Wealsoderivedthecoronalmagneticconfigurationsoftherelatedsolaractiveregions(ARs)fromthepotential-fieldsource-surface(PFSS)model. Itisfoundthat: (1)11ofthe12openmagneticfield-lineeventsareprompteventswhoseparticlereleasetimescoincidewiththemaximaofflareemission. 13ofthe14closedmagneticfield-lineeventsaredelayedones, theexceptionalprompteventisassociatedwithalarge-scalecoronaldisturbanceordimming. (2)Anaveragedharderspectrumisfoundinopenmagneticfield-lineeventscomparedwiththeclosedones. Additionally, anobvioushigherrolloverenergyisseeninclosedmagneticfield-lineeventscomparedwiththeopenones. Thesecorrelationsclearlyestablishasignificantlinkbetweenthecoronalmagneticfield-linetopologyandtheescapeofchargedparticlesfromthesolarAR intointerplanetaryspaceduringthemajorsolarenergeticparticle(SEP) events.
StochasticParticleAccelerationbyCompressiveModeswithIncompressiveModeInducedSpatial
DiffusionSimingLiu (UniversityofGlasgow)with
Lyndsay Fletcher, and Eduard Kontar
Theinteractionbetweenlarge-scaleplasmafluctuationsandenergeticparticlesisoftenbelievedtobetheprocessresponsibleforparticleaccelerationinvariousastrophysicalsituations.Non-resonantstochasticinteractionsofparticleswithlarge-scalecompressivewavemodesleadtosecond-orderFermiacceleration. Thedetailsofthisaccelerationdependnotonlyonthespectrumofthecompressivemodesbutalsoontheparticlespatialdiffusioncoefficient. Sinceincompressivemodesaremoreefficientthancompressivemodesinscatteringoftheparticlesforthecompressivewavespeedhigherthantheincompressiveeddyspeed, boththecompressibleandincompressiblemodesplaycrucialrolesindeterminingtheresultantparticledistribution. Wewillreportouron-goinginvestigationofstochasticparticleaccelerationbyaspectrumofcompressiveandincompressivemodes. ThisworkissupportedbytheEU'sSOLAIRE ResearchandTrainingNetworkattheUniversityofGlasgow(MTRN-CT-2006-035484).
FromelectronmapstoaccelerationmechanismsofenergeticparticlesintheflaringSun
MichelePiana (Universita'diGenova)withA. GordonEmslie(OklahomaStateUniversity),
and Massone(CNR - SPIN),and Anna Maria(CNR- SPIN)
Imagingspectroscopyinvolvesinversionofbothspatialandspectraldatatoyield‘insitu’informationonthesourceasafunctionofbothenergyandposition. Inthespecialcasewherethespatialinformationisencodedintheformofvisibilities(two-dimensionalspatialFouriertransformsofthesourcestructure)itis
advantageous, bothconceptuallyandcomputationally, toperformfirstthespectralinversion, whichyieldsvisibilitiesoftheunknownsourcefunction; andthentospatiallytransformthesesourcefunctionvisibilities, whichyieldsmapsofthesourcefunctionatdifferentenergies.ForthevisibilitiesobservedbytheReuvenRamatyHighEnergySolarSpectroscopicImager(RHESSI)thisapproachhasbeenappliedforimagingspectroscopyanalysisofhardX-rayemissionduringsolarflares. Thisprocedureinvolves:regularizedinversionofthecountvisibilityspectratoobtainsmoothedformsofthecorrespondingelectronvisibilityspectra; applicationofconventionalvisibility-basedimagingalgorithmsthatyieldsimagesoftheelectronfluxthatvarysmoothlywithenergy.
ThepresenttalkwillshowhowsuchanapproachcanbeutilizedtoinferquantitativeinformationontheaccelerationmechanismsoccuringinsolarplasmaduringtwoflaringeventsobservedbyRHESSI.Morespecifically, inthecaseofthesolarflareobservedonFebruary202002, wewillshowthatRHESSI dataareconsistentwithCoulombcollisionsbetweenanaccelerationsitehighinthecoronaandthedensechromosphericfootpointregions; andthatananalysisofthecentroidpositionsoftheseelectronmapsallowsustoinferthedensitystructureinthetwovisiblecompactsources. Then, fortheNovember032003solarflare, wewillshowhowPetrosianandChen(2010)couldusethismethodandthehigh-resolutionX-rayobservationsprovidedbyRHESSItoderiveseveralimportantparametersofthestochasticmodelforparticleacceleration.
Electromagneticemissionfrombeam-generatedLangmuirwaves
HeatherRatcliffe (UniversityofGlasgow)
Thebeamsofflare-acceleratedelectronsinthesolarcoronahavebeenextensivelystudiedandareknowntoproducehighlevelsofLangmuirwaves.Thesemayinturnproduceelectromagneticemission, boththroughscatteringbythermalionsintheplasma, orbya3-wavedecayprocessinvolvingion-soundwaves. Bothoftheseproduceradiationneartheplasmafrequency, andarepossiblemechanismsforTypeIII radioemissionneartheplasmafrequency. Becausethelatterrequiresappreciablelevelsofionsoundwavestobepresentitisonlyofinterestwheretheelectrontemperaturefarexceedstheiontemperature; theformermayoccurwhentheiontemperatureissimilar, orgreaterthan, theelectrontemperature.Thesituationmaybetreated1-dimensionally, byassumingthetransversewavesareemittedperpendiculartotheLangmuirwaves. Thekineticequationscanthenbesolvednumerically, usingafirstorderfinitedifferenceintegrationscheme; thisisdoneforahomogeneousplasmaatadensitytypicalofthesolarcorona.Someresultsforthespectrumofplasmaemissionarepresentedforvaryingvaluesoftheelectronandiontemperatures, anddifferentfunctionalformsfortheinitialLangmuirwavespectrum.
SolarFlareAcceleratedElectronTransportthroughtheTurbulentDensityoftheSolarWind
HamishReid (UniversityofGlasgow)withEduard Kontar
SolarflareacceleratedelectronbeamspropagatingawayfromtheSuncaninteractwiththeturbulentinterplanetarymedia, producingplasmawavesandtypeIII radioemission. TheseelectronbeamsaredetectedneartheEarthwithadoublepower-
P19 69
lawenergyspectra. WesimulateelectronbeampropagationfromtheSuntotheEarthintheweakturbulentregimetakingintoaccounttheself-consistentgenerationofplasmawavesandsubsequentwaveinteractionwithdensityfluctuationsfromlowfrequencyMHD turbulence.Therateatwhichplasmawavesareinducedbyanunstableelectronbeamisreducedbybackgrounddensityfluctuations, mostacutelywhenfluctuationshavelargeamplitudesorsmallwavelengths. Thissuppressionofplasmawavesaltersthewavedistrubtionwhichchangestheelectronbeamtransport. Assuminga5/3Kolmogorov-typepowerdensityspectraoffluctuationsoftenobservedneartheEarth, weinvestigatethecorrespondingenergyspectraoftheelectronbeamafterithaspropagated1AU.Wefindadirectcorrelationbetweenthespectraofthedoublepower-lawbelowthebreakenergyandtheturbulentintensityofthebackgroundplasma. Foraninitialspectralindexof3.5, wefindarangeofspectrabelowthebreakenergybetween1.7-2.1,withhigherlevelsofturbulencecorrespondingtohigherspectralindices.
Numericalsimulationofmagnetosphericelectroncyclotronemission
DavidSpeirs (DepartmentofPhysics, UniversityofStrathclyde)with K. Ronald, K.M. Gillespie,S.L. McConville, A.D.R. Phelps, A.W. Cross,
R. Bingham, B.J. Kellett, R.A. Cairns, and I. Vorgul
Whenaninitiallymainlyrectilinearelectronbeamissubjecttosignificantmagneticcompression,conservationofmagneticmomentresultsintheformationofahorseshoeshapedvelocitydistribution. Ithasbeenshownthatsuchadistributionisunstabletocyclotronemissionandmayberesponsibleforthegenerationofplanetaryandstellarauroralradioemissions. Principlecharacteristicsofsuchemissionsincludeahighdegreeofextraordinary(X) modepolarizationandaspectraloutputcomprisingwelldefinedcomponentsextendingdowntoalowerfrequencycut-offcorrespondingtothelocalrelativisticelectroncyclotronfrequency. PiC codesimulationshavebeenundertakentoinvestigatethedynamicsofthecyclotronemissionprocessintheabsenceofradiationboundarieswithparticularconsiderationofthespatialgrowthrate,spectraloutputandRF conversionefficiency.Computationsrevealthatawell-definedcyclotronemissionprocessoccursalbeitwithareducedspatialgrowthratecomparedtowaveguideboundedsimulations. RF outputisnearperpendiculartotheelectronbeamwithaslightbackward-wavecharacterthatisalsoreflectedinthespectraloutput. ThecorrespondingRFconversionefficiencyof1.1%iscomparabletowaveguideboundedsimulationsandconsistentwiththepredictionsofkinetictheorythatsuggestefficient, spectrallywelldefinedemissioncanbeobtainedfromanelectronhorseshoedistributionintheabsenceofradiationboundaries.
MagnetosphericParallelElectricFieldsCraigStark (UniversityofSt. Andrews)with
A.N. Wright, and A.P. Cran-McGreehin
Field-alignedcurrentsobservedalongtheEarth’smagneticfieldcoupletheionospheretothemagnetosphere. Suchcurrents, andtheirassociatedparallelelectricfields, areresponsiblefortheobservedauroraandplayasignificantroleintheglobalcurrentnetworksurroundingtheEarth. Byconsideringthemotionoftheiono-magnetosphericplasma, undertheinfluenceofabackgroundelectromagneticfield, onecanobtain
aquasi-steadystateelectricfielddistributionalongthemagneticfieldwhilepreservingquasi-neutrality. Theaimofthisresearchistounderstandhowtheimplicatedplasmasrespondtothesefields, howthisvarieswithspeciestemperature, theprescribedelectricfieldstrengthandaltitude. Wepresentaplasmakinetictreatment, analysinghowthevelocitydistributionfunctionsevolvealongamagneticfluxtube,takingintoaccountmirroringandprecipitatingpopulations. Bycalculatingthemomentsoftheresultingdistributionfunctionsweascertainhowthecollectiveelectromagneticandpressureeffectsactingontheplasmaarebalancedandmaintained, establishingadynamicequilibrium.Herewediscussourkineticplasmamodelandpresentwork-in-progress, preliminaryresults.
Electronsre-accelerationatthechromosphericfootpointsofSolarFlares
RimTurkmani (ImperialCollege)with John Brown,Eduard Kontar, Alec MacKinnon, and
Loukas Vlahos
Traditionallyacceleratedelectronsinsolarflaresarethoughttobeacceleratedinthecoronalpartoftheloop, andthentraveltothefootpointswheretheylosetheirenergyandradiatetheobservedHardX-ray. Werevisitthisassumptionbackedwithincreasingobservationalevidencethatchallengesthissimplifiedpicture. WeproposeanewLocalRe-accelerationThickTargetModel(LRTTM) whereatthefootpointselectronsreceiveaboostofre-accelerationinadditiontotheusualcollisionalloses. Suchmodelmayofferanalternativetothe‘standard’collisionalthicktargetinjectionmodel(TTM) (Brown1971)ofsolarHXRburstsources, requiringfarfewerelectronsandsolvingsomerecentproblemswiththeTTMinterpretation. Welookatthedifferentscenariosthatcouldleadtosuchre-accelerationandpresentnumericalresultsfromoneofthem.
AuroralParticleAccelerationattheEarthAndrewWright (UniversityofStAndrews)
Anoverviewisgivenoftheoriginofparticleaccelerationintheterrestrialauroralcurrentsystem. Theseparticlesareimportantincouplingthemagnetospheretotheionosphereviaelectricalcurrentsthatflowalongmagneticfluxtubes, andarealsoresponsibleforproducingthevisibleaurora. Examplesofspacecraftparticledatawillbeusedtoillustratesomeofthemainaccelerationmechanisms.
P20TheGRB-SN connection: ExploringGRB
progenitorswithmulti-wavelengthobservationsZachCano (ARI,JohnMooresUniversity
Liverpool)
OveradecadeagotheGRB-SN connectionwashintedat, andlaterconfirmedspectroscopicallyin2003. Duringthisperiodithasbeenshownthatatleastsome, ifnotalllong-durationGRBsarecausedbythecore-collapseofamassivestarintoatypeIcSN.AlthoughanabsoluteconnectionofaGRB toaSN canonlybedonespectroscopically,photometricevidenceofSN "bumps"inGRB LCsthatareaccompaniedbyachangeincolourprovidecircumstantialevidenceforaconnectionbetweenGRBsandthecollapseofmassivestars.
Usingdatatakenonnumeroustelescopes,includingseveralepochsonHST,threelinesofevidenceareprovidedforaconnectionofaredSN withGRB 060729. SN "bumps"areseeninthelight-curvesthatareaccompaniedbyachangeincolour, andatlatetimesthespectrumoftheOTresemblesthatofthearchetype1998bw, onlyredder.
FurtherevidenceisalsogivenforanassociationofaSN withGRB 090618. A beautifully-detailedandwell-sampledlight-curvehasbeenobtained,andredSN "bumps"areseen. ThoughbothoftheGRBsarelocatedatthesamecosmologicaldistance(z=0.54), theSNeappeardifferent. TheseresultsfurthervindicatetheGRB-SN connection,concludingthatwhileaGRB islikelyformedduringthecollapseofamasivestar, theresultingSNearesubstantiallydifferent.
GRB090510, thefirstcasestudyofashortGRBwithGeV extendedemissiondetectedbyFermi
andSwift.MassimilianoDePasquale (UniversityCollege
London–MSSL) with SwiftTeam, FermiGBMCollaboration, and LAT Collaboration
Thebright Γ−RayBurstGRB 090510wasunprecedentedasthefirstshortGRB detectedsimultaneouslybySwift-XRT &UVOT andFermi-LAT,coveringtheenergyrangefrom0.002keV tomorethan300GeV.ExtendedGeV emissionwasdetectedbyFermi-LAT,lastingfor200saftertheinitialtrigger, andityieldedthehighestenergyphotoneverobservedfromashortGRB (30.5GeV).Wereportonthejointmulti-wavelengthobservationsofGRB 090510performedbyFermiandSwift. ThisexceptionalGRB enabledustoinvestigatethephysicalpropertiesoftheGRBoutflow, poorlyunderstoodinshortbursts. Wediscussinternalandexternalshockmodelsforthebroadbandenergyemissionofthisobject.
Identifyingandchacterisingtheprogenitorsofcore-collapsesupernovae
MorganFraser (QueensUniversityBelfast)withA. Pastorello, S. Smartt, and K. Takats
Core-collapsesupernovae(SNe)arethespectacularend-pointsofstellarevolution. Notonlyaretheyakeytestforstellarevolutionarymodels, buttheyarealsoanopportunitytostudythephysicsunderlyingsomeofthemostenergeticeventsintheUniverse. DetectingtheprogenitorsoftheseSNeinarchivalimagesallowsustodirectlylinkmassivestarstosupernovae, andindoingso, tounderstandhowthepropertiesoftheprogenitor(mass, metallicityetc.) affectthecharacteristicsandevolutionofthesupernova, andultimatelyleadtothedifferentsupernovasubtypes.
Wepresentrecentresultsfromoursupernovaprogenitorprogram, focusinginparticularontheTypeII SN 2009kr, whereweidentifyacandidateprogenitorinarchivaldatafromtheHubbleSpaceTelescope. Thecandidatewefind, ifasinglestar,isconsistentwithayellowsupergiantprogenitor,whichisincontrasttotheredsupergiantprogenitorfoundforallotherTypeIIP SNesofar.
HighlightsfromFermiobservationsofGamma-RayBursts
JonathanGranot (UniversityofHertfordshire)
TheFermi Γ−RaySpaceTelescopehasmorethandoubledthenumberof Γ−RayBursts(GRBs)detectedathighenergies(> 100 MeV) withinitsfirstyearofoperation. Thankstotheverywide
70 P19–P20
energyrangecoveredbyFermi's Γ−rayBurstMonitor(GBM;8keV to40MeV) andLargeAreaTelescope(LAT;25MeV to > 300 GeV) ithasmeasuredthepromptGRB emissionspectrumoveranunprecedentedlylargeenergyrange(from∼ 8 keV to ∼ 30 GeV).I willpresenthighlightsofFermiGRB observationsoveritsfirst1.5yearsofoperation, focusingmainlyonthepromptemissionphase. Interestingnewobservationswillbediscussedalongwithsomeoftheirpossibleimplications, including:
(i)WhatcanwelearnfromtheFermi-LAT GRBdetectionrate,
(ii)A limitonthevariationofthespeedoflightwithphotonenergy(forthefirsttimebeyondthePlanckscaleforalinearenergydependencefromdirecttimeofarrivalmeasurements),
(iii)Lower-limitsonthebulkLorentzfactoroftheGRB outflow(of ∼ 1000 forthebrightestFermiLAT GRBs),
(iv)Thedetection(orinothercases, lackthereof)ofadistinctspectralcomponentathigh(andsometimesalsoatlow)energies, andpossibleimplicationsforthepromptGRB emissionmechanism,
(v)Thelateronset(andlongerduration)ofthehigh-energyemission(> 100 MeV) comparedtothelow-energy(< 1 MeV) emissionthatisseeninmostFermi-LAT GRBs.
Discoveryofanunusualnewradiosourceinthestar-forminggalaxyM82: Faintsupernova,
supermassiveblackhole, oranextra-galacticmicroquasar?
TomMuxlow (JodrellBankCentreforAstrophysics)with Rob Beswick, Simon Garrington, Alan Pedlar,
Danielle Fenech, Megan Argo,Janinevan Eymeren, Martin Ward, Andreas Zezas,
and Andreas Brunthaler
A faintnewradiosourcehasbeendetectedinthenuclearregionofthestarburstgalaxyM82usingMERLIN radioobservationsdesignedtomonitorthefluxdensityevolutionoftherecentbrightsupernovaSN2008iz. Thisnewsourcewasinitiallyidentifiedinobservationsmadebetween1-5thMay2009buthadnotbeenpresentinobservationsmadeoneweekearlier, orinanypreviousobservationsofM82. Inthispaperwereportthediscoveryofthisnewsourceandmonitoringofitsevolutionoveritsfirst9monthsofexistence. Thetruenatureofthisnewsourceremainsunclear, andwediscusswhetherthissourcemaybeanunusualandfaintsupernova, asupermassiveblackholeassociatedwiththenucleusofM82, orintriguinglythefirstdetectionofradioemissionfromanextragalacticmicroquasar.
Searchforgravitational-waveinspiralsignalsassociatedwithshortGamma-RayBurstsduring
LIGO'sfifthandVirgo'sfirstsciencerunValeriuPredoi (CardiffUniversity)with LIGO
ScientificCollaboration, and VirgoCollaboration
Oneofthemostcommonlyacceptedcandidatesourcesforshorthard γraybursts(SHB) isthemergerofcompactbinaryobjects, i.e. eitherneutronstar-neutronstarorneutronstar-blackholebinarysystems. Suchmergersarealsopredictedtoemitstronggravitationalradiationwithwaveformsthatcanbedescribedtheoretically. Wepresentasearchfortheseknowngravitational-wavesignaturesintemporalanddirectionalcoincidencewith22SHBsdetectedby γraytelescopesduring
LIGO'sfifthsciencerun, S5, andVirgo'sfirstsciencerun, VSR1. Thedatareductionpipelinemakesuseofmatchedfilteringofthegravitationalwavedetectoroutputagainstatheoreticalwaveformtemplatebank. Wefindnostatisticallysignificantgravitational-wavecandidateswithina[-5, +1)swindowaroundthetimeofanyGRB.Usinganadequatestatisticaltest, wefindnoevidenceforanexcessofweakgravitational-wavesignalsinoursampleofGRBs. Weexcludeneutronstar-blackholeprogenitorstoamedian90%CL exclusiondistanceof6.7Mpc.
DiscoveryoftheafterglowandhostgalaxyofthelowredshiftshortGRB 080905A
AntoniaRowlinson (UniversityofLeicester)withK. Wiersema, A.J. Levan, N.R. Tanvir, P.T. O'Brien,
andothers
WepresentthediscoveryofshortGRB 080905A,itsopticalafterglowandhostgalaxy. InitiallydiscoveredbySwift, ourdeepopticalobservationsenabledtheidentificationofafaintopticalafterglow, andsubsequentlyaface-onspiralhostgalaxyunderlyingtheGRB position. Furthermorethereisnosupernovacomponentpresentintheafterglowtodeeplimits. Spectroscopyofthegalaxyprovidesaredshiftofz=0.1218, thelowestredshiftyetobservedforashortGRB.TheGRB liesoffsetfromthehostgalaxycentreby ∼ 18.5 kpc,inthenorthernspiralarmwhichexhibitsanolderstellarpopulationthanthesouthernarm. Noemissionlinesarevisibledirectlyundertheburstposition, implyinglittleongoingstarformationattheburstlocation. ThesepropertieswouldnaturallybeexplainedweretheprogenitorofGRB080905A acompactbinarymerger.
LuminoustransientsinthedistantuniversewithPTF andSNLS
MarkSullivan (UniversityofOxford)
TheSupernovaLegacySurvey(SNLS) andthePalomarTransientFactory(PTF) arebothrollingtransientsurveys, designedtosurveydistantcosmicexplosionswithoutregardtohostgalaxytypeorenvironment, andarethusfreefromthebiasesassociatedwithearliergalaxy-targetedprogrammes. Bothsurveysareuncoveringnewtypesandexamplesofsupernovaexplosionswithunprecedentedultra-violetluminosities, locatedatsomeofthehighestredshiftsyetdiscovered. Inthistalk, I willpresentthelatestresultsonthistopicfrombothsurveys.
InvestigationoftheenvironmentofshortgammarayburstGRB090510withaviewtoconstraining
theprojenitor.RachelTunnicliffe (UniversityofWarwick)with
A. Levan
Investigationoftheenvironmentsoflong ΓRayBursts(GRBs)hasshownthemtobeassociatedwithmassivestarsandhencehasgonesomewaytoidentifyingtheirprojenitors. A similarprocedureisrequiredforshort, hardburstsofwhichtherearefewerwellobservedeventsmeaningafullinvestigationofeveryburstisimportant. WehaveanalysedtheburstandenvironmentofGRB 090510, basedonNOT andVLT observations. ThisburstwasalsospectacularlydetectedbyFermiouttoenergiesinexcessof30GeV.Becauseofthis, italsoprovidesunprecedentedinsightintopossibleLorentzInvarianceViolations, althoughthisdependscruciallyontheknownburstredshift. Usingtheopticalafterglowwepinpointthelocationofthebursttooccurringsome7kpcfromthecoreofa
quiescentgalaxyatz=0.903. Thecharacteristicsofthishost, andtheoffsetoftheburstfromit, areinconsistentwiththepropertiesoflongGRBs, butbroadlyconsistentwiththoseofthesmallsampleofshortGRB hosts. ThisisinkeepingwiththeexpectationsofmodelsfortheproductionofshortGRBsincompactbinarymergers.
P21TeVeS andthestraightarcofA2390
MartinFeix (UniversityofStAndrews)withHongsheng Zhao, Cosimo Fedeli,
JoséLuisGarrido Pestaña, and Henk Hoekstra
Wesuggesttotestthecombinedframeworkoftensor-vector-scalartheory(TeVeS) andmassiveneutrinosingalaxyclustersviagravitationallensing, choosingthesystemA2390withitsnotoriousstraightarcasanexample. Adoptingquasi-equilibriummodelsforthemattercontentofA2390, weshowthatsuchconfigurationscannotproducetheobservedimage. Generally, nonlineareffectsinducedbytheTeVeS scalarfieldareverysmall, meaningthatcurleffectsarebasicallynegligible. Basedonthisresult, weoutlineasystematicapproachonhowtomodelstronglensesinTeVeS,whichisdemonstratedforA2390.Comparedtogeneralrelativity, weconcludethatdiscrepanciesbetweentheindependentmassestimatesfromlensingandX-rayobservationsareamplified. Finally, weaddressthequestionofthemodel’sfeasibilityandpossibleimplications/problemsforTeVeS.
Thenewpathtotimedelays?GülayGürkan (TheUniverstiyofManchester)with
Neal Jackson
Tobetterunderstandtheuniverseanditsdynamics, theHubbleconstantisacrucialparameterwhichprovidesvaluableinformationabouttheexpansionrateoftheuniverse. Sofar,theHubbleconstanthasbeendeterminedbyvariousmethodssuchasCepheidvariablesbyutilizingHST KeyProjectdataandWMAP.TheaccuracyoftheHubbleconstantvalueisnotbetterthan10%duetointrinsicconstraints/assumptionsofeachmethod.
GravitationallenssystemsprovideanotherprobeoftheHubbleconstantusingtimedelaymeasurements. CurrentinvestigationsoftimedelaylenseshaveresultedindifferentvaluesofHorangingfrom50-80km/s/Mpc. Themainproblemingravitationallenssystemsisthatrequiresamassmodelforthelenswhichisdifficulttomeasureindependentlyunlessobservationalconstraintsareavailable. Moreover, inordertoseetimedelaysclearly, fluxesofsourceshavetobevariable. Ontheotherhand, usingatypicalvalueoftheHubbleconstantandmeasuredtimedelaysenableustodetermineabetter/moreaccuratemassmodelforthelensgalaxy.
Hereweattempttodevelopanewandmoreefficientmethodformeasuringtimedelays, whichdoesnotrequireregularmonitoringwithahigh-resolutioninterferometerarrayorwithopticaltelescopes. Instead, theWSRT isusedforfluxmonitoringofdoubleimagelenssystemsinwhichthebrighterimageisexpectedtovaryfirst.TriggeredVLA observationscanthenbeusedtocatchthesubsequentvariabilityofthefainterimage. Wepresentpreliminaryresultsfromsuchaprogram.
P20–P21 71
ProbingtheDarkUniversewithWeakLensingTomographyandtheCFHTLS
CatherineHeymans (IfA,UniversityofEdinburgh)with Emma Grocutt, Alan Heavens, Tom Kitching,
and CFHTLenS team
Weakgravitationallensingisapowerfultechniqueformeasuringthepropertiesofdarkmatteranddarkenergyfromtheirgravitationaleffectsalone.TheCanada-France-HawaiiTelescopeLegacySurveyiscurrentlythelargestdeepopticaldatasetforweaklensinganalysiscovering172squaredegreesover5opticalbands. Wepresentaninvestigationintotheoptimaltomographicthree-dimensionalanalysisoftheCFHTLS weaklensingsignalthatminimisestheimpactofsystematicsarisingfromintrinsicgalaxyalignments. Withsystematicsundercontrol, sincetheinfluenceofdarkenergyonstructuregrowthisredshift-dependent, tomographicanalysisofredshiftbinswillallowustoconstrainthepropertiesoftheDarkUniverse.
ApplicationsofaNewandRapidSimulationsMethodforWeakLensingAnalysis
AlinaKiessling (UniversityofEdinburgh)withAndy Taylor, and Alan Heavens
Gravitationallensingissensitivetoallgravitatingmass- bothBaryonicandDarkMatter- makingittheidealtooltostudyCosmologyindependentlyofanyassumptionsaboutthedynamicalorthermalstateofobjects. TheNextGenerationofSurveyTelescopewillobservemoreoftheskythaneverbeforeandthevolumeofdatatheywillproduceisunprecedented. Torealisethepotentialofthesesurveys, experimentsrequirefulllargeend-to-endsimulationsoftheSurveystotestanalysismethodsandproviderealisticerrors. Wehavedevelopedanewline-of-sightintegrationapproachtosimulating3-D WeakGravitationalLensShearandConvergencefields. Theselightconesarefastertogeneratethantraditionalray-tracing, sowecanrunanensembleofsimulationsallowingustogeneratecovariancematriciesforcosmologicalparameterestimationandstatisticalanalysis. Thispresentationwillintroduceournewanalysismethodanddiscusssomeofitsmanyapplicationsinweaklensingexperiments.
UsingtheLHC toprobeDarkMatterinphysicsbeyondtheStandardModel
DavidMiller (UniversityofGlasgow)
Ourextremelysuccessfulmodelofparticlephysics, theStandardModel, hasaprofoundflaw:ithasnoviablecandidatefordarkmatter. Inordertoincorporatedarkmatterintoourpictureoftheuniverse, wemustgobeyondtheStandardModeltotheoriessuchassupersymmetryorextradimensions. Ourcurrentdataindicatesadarkmattercandidatewithanelectroweakscalemass,exactlytherangethatwillbeprobedbythenewLargeHadronCollider(LHC).InthistalkI willreviewmodelsbeyondtheStandardModelthatprovideaviabledarkmattercandidateanddiscussthepotentialfortheirdiscoveryattheLHC.
BrightIdeasandDarkThoughts: "UniversalBaryonicScale"at"MaximumHaloGravity"
HongshengZhao (U.ofStAndrews(SUPA)) withGianfranco Gentile, Benoit Famaey, Paolo Salucci,
Andrea Maccio, Baojiu Li, Henk Hoekstra, andMartin Feix
I willinterpretaverycuriousconspiracyofdark-brightmatteringalaxies(Gentileetal2009Nature), insensitivetothesizesandformation
historiesoftheobservedgalaxies: thebaryonsareconcentratedtoapproximatelythesamesurfacedensityattheverypositionwherethehaloofferslocallymaximumgravity. Whilenormalgravitationalandgasfeedbackprocessesmustalwaysoccur, itisdifficulttoforgeafeedbackhistory-independentuniversalscaleunlessthereissomehelpfrompossiblynewphysicsintheDark.A partialconfirmationisseeninsimulationsofN-bodywherethematteriscoupledtoacosmologicalscalarfield(Zhaoetal. 2009, ApJLetters).
P22ImagingwithMIRC attheCHARA interferometer
FabienBaron (UniversityofMichigan)withJohn Monnier, Stefan Kraus, and Xiao Che
WepresenttherecentresultsobtainedwiththeMichiganInfraRedCombiner(MIRC) operatingattheCHARA interferometeratMountWilson, CA.Bycombininglightfromuptofourtelescopessimultaneously, MIRC allowsfastandmodel-independentimagingofstellarsurfacesorstellarsytemsatresolutionsbelowonemilliarcsecond.AmongsttheimagedobjectsaretherapidrotatingstarsAltairandAlderamin, thefamousinteractingbinariesBetaLyraeandAlgol, andthepeculiareclipsingsystemEpsilonAurigae. FinallyimagingYoungStarObjectswillbeattemptedaspartofthenextMIRC campaign, exploitingthepowerofthenew6-telescopefringe-trackingcapabilities.
ThecomplexinnerdisksofHerbigAeBestarsMyriamBenisty (INAF - Arcetri)with A. Natta,
A. Isella, E. Tatulli, F. Ménard, J.P. Berger, F. Massi,and F. Malbet
Understandingthephysicalconditionsintheclosecircumstellarenvironmentsofyoungstarsisacrucialsteptocomprehendplanetformationandevolution. Inthistalk, I willdiscussnear-infraredspectro-interferometricobservationsofHerbigAeBestars, thatallowedustodirectlyprobethehotcircumstellargasanddust. Thestructureoftheirinnermostregionshasbeenwidelydebatedandinthepastdecade, thegeneralconsensushasbeenthattheobservednearinfraredexcessisduetodirectthermalemissionfromhotdustlocatedattheirsublimationradius, inapuffed-uprim. Inthistalk, I willfirstpresenttwocasesthatsuggestthatthisdescriptionismaybetoosimple. I willshowlong-baselinespectro-interferometricobservationsoftheHerbigAestarHD163296obtainedwiththeAMBER instrumentattheVLTI,resultinginthelargestUV coverageachievedonayoungstartoday. Modelfittingofphotometricandinterferometricobservationssuggeststhatadominantcontributiontothenear-infraredemissionarisesfromanopticallythinregionextendingfromabout0.10to0.45AU,distancefromthestaratwhichanopticallythickdustydiskstarts. I willdiscussthenatureofthisemissionandwillarguethatitcouldtracethepresenceofveryrefractorygrainsratherthangas. I willalsopresentthecaseofHD100546, anoldHerbigBestar,thoughttohaveatransitionaldiskwithagap.Radiativetransfermodellingofthephotometricandinterferometricobservationsconfirmedthepresenceofthegap, constrainedthetotalmassofdustlocatedinsideitsinneredge, andallowedageneralstructureforthisevolveddisktobederived. Althoughgenerallyneglected, thisstudy,inaddition, showsthatscatteredthermallightcan
havealargecontributiontothenear-infraredcontinuumemission.
ScienceProspectswiththeMagdalenaRidgeObservatoryInterferometer(MROI)
DavidBuscher (UniversityofCambridge)withChris Haniff, and John Young
TheMagdalenaRidgeObservatoryInterferometerisanoptical/infraredaperturesynthesisinterferometerdedicatedtoimagingfaintobjectsatresolutionsdownto300micro-arcseconds. Itisbeingbuiltatahigh-altitudesiteinNewMexicobyapartnershipbetweentheUniversityofCambridgeandNewMexicoTech. Wegiveanoverviewofthetypesofhigh-angular-resolutionsciencethatMROI istargeting, includingstellarastrophysics, YSO disksandplanetformation, andAGN astrophysics. Wepresentanupdateonprogressonconstructionandanear-termtimelinefortheinterferometer.
ImagingshockfrontsinMiravariablesJamesGordon (UniversityofCambridge)with
David Buscher, and John Young
WediscusstheuseofhighangularresolutionopticalinterferometryforimagingshockfrontspropagatingthoughtheatmosphereofMiravariables. HighresolutionspectroscopyhaspresentedstrongevidencefortheexistenceofasupersonicshockevidentinBalmeremissionlines. Aperturemaskingandluckyimagingintheemissionlineatdifferentpulsationphaseswillallowustoreconstructimagesoftheshockfront.UnderstandingthepropertiesoftheshockisessentialforatmosphericmodelsandthecalculationofmasslossrateswhichhavedifficultyinaccountingforshocksinMiravariables.
DustydiscsaroundevolvedstarsFoteini(Claire)Lykou (JodrellBankCentrefor
Astrophysics)with Albert Zijlstra, andOlivier Chesneau
Wepresentthediscoveryofdusty, edge-ondiscsaroundevolvedstarsatdifferentevolutionarystages. Menzel3, M2-9andSakurai’sObjectwereobservedwithMIDI ontheVeryLargeTelescopeInterferometer(VLTI) providingaresolutionof∼ 0.01 arcsecinthemid-infrared. Thefirsttwoobjectscontaindiskscomposedofsilicatedust,whilethelastcontainsadisc-likestructureofcarbonaceousmaterial. Thedustydiscsarealignedwiththeminoraxisofthebipolarnebulae(oradensityenhancementontheroundnebulaforthelastobject)andtheirinnerrimradiiarelessthan100AU.Characterisingthedustydiscsinthecoreofthesenebulaeandatdifferentevolutionarystages, providesinvaluableconstraintsontheprocessesthatleadtotheseimpressivenebulae.Thepropertiesofeachdischavebeenexploredwiththemeansofradiativetransfermodelling.
Opticalandnear-infraredinterferometryofstarsanddisks
ReneOudmaijer (UniversityofLeeds)
Theseareexcitingtimesforopticalandnear-infraredinterferometry. Itisonlyinthelastfewyearsthatspectrallyresolvedinterferometryatmilli-arcsecondscaleshasbecomepossibleonaregularbasis, andthefuturepromisesevenmore.InthistalkI willreviewthelatestinterferometricresultsonbothyoungandevolvedstars.
72 P21–P22
InvestigatingtheinnerdisksofyoungstarsJennyPatience (UniversityofExeter)with A. Binks,
R. Rhodes, and R. Akeson
WiththeexceptionalangularresolutionoftheKeckinterferometer, wearestudyingtheinnerdisksofyoungstarsatdifferentevolutionarystagesatspatialscalesoflessthan1AU.Thevisibilitiesofseveraltargetsindicatetheinnerdiskshavebeenspatiallyresolved. Thesizesoftheinnerdisksareestimatedbasedonmodelfitsandarecomparedwiththeexpectedradiusofdustsublimation, consideringtheluminosityofeachobject. Theestimatedinnerdiskradiioftheyoungstarsarealsocomparedwiththedistributionofcloseorbitextrasolarplanetstoinvestigateimplicationsforplanetmigration.
Mappingstar-spotsontheRS CVnbinary ζ AndEttorePedretti (SUPA,UniversityofStAndrews)with John Monnier, AndrewCollier Cameron,
Jean-Francois Donati, and Pascal Petit
WeobservedthemagneticallyactiveRS CVnbinaryZetaAnd=HD 4502usinglong-baselineinterferometryinordertodeterminethepolarspotstructure, whichhasbeendetectedbyZeeman-DopplerspectroscopyinseveralRS CVnbinaries.ThestarisanellipsoidalK giantbinarywhichhasbeenrecentlyimagedusingtheZeeman-Dopplertechnique. ThestarwasobservedattheCHARAinterferometerinAugust2007and2008. Theobtainedimagesshowasurfacewithasymmetricfeaturesconsistentwithstarspots.
TheMagdalenaRidgeInterferometerFringeTracker
AlexRea (UniversityofCambridge)withC. Jurgenson, F. Santoro, T. McCracken,
A. Olivares, D. Buscher, M. Creech-Eakman,C. Haniff, J. Young, A. Shtromberg, K. McCord,
and F. Baron
TheMagdalenaRidgeObservatoryInterferometer(MROI),acollaborationbetweenNewMexicoTechandtheUniversityofCambridge, willperformhigh-resolutionimagingdowntoalimitingmagnitudeofH=14. WereportonthestatusoftheMROI fringetracker, whoseperformancewillbecriticaltoreachingthislimitingsensitivity. Designoftheinstrumentiscomplete, andthefringetrackerisnowunderconstructionatMRO.Itconsistsofadedicated,near-IR,fringe-trackingbeamcombinerandspectrographs. Theinstrumentwillphaseuptheinterferometerbystabilizingfringesontheshorter"nearestneighbor"baselinesofthe"Y"-geometryarray, allowingforincreasedintegrationtimesonthelongerbaselinesandthebuildupofsignal-to-noiseinthescienceinstrument. Thebeamcombinerhasbeendesignedtoacceptlightfromamaximumoftentelescopes(threeoneacharrayarm, oneatthe"Y"vertex), butcanoperatewithfewerwithouthavingtochangetheoveralllayout.Eachspectrographwillmultiplexuptofivebeamcombineroutputsontoasingledetector. A pairofidenticalspectrographsareusedtosimultaneouslysamplecomplementaryfringepatternsthatareπradiansoutofphasewitheachother, reducingthenumberofmodulatorstepsneededtomeasurethefringephase.
Dosingleoldstarsejectclumps?AnitaRichards (JBCA,UniversityofManchester)with Indra Bains, Phil Diamond, Malcolm Grey,
Graham Harper, Jeremy Lim, Dinhvan Trung, andJeremy Yates
Radiointerferometricimagingofatsub-AUresolutionshowsthatthewindsaroundevolvedstarsarecurdledintoclumps. Inthezonewheredustformationiswelladvanced(&5stellarradii),outtomanytensR*, thewatermasercloudsareover-denseand, ifextrapolatedbacktothestellarsurface, theirbirthsizeswouldhavebeenoforder0.1R*. Istheclumpingscalesetbystarspots,possiblyrelatedtoconvectioncells? Thisraisestheintriguingpossibilitythatthechemistryaswellasthedensitycouldbedifferentiatedintheclumps.Alternatively, ifthepulsation-poweredmass-lossprocessissmooth, cloudsmightbearesultofdustformation. Interferometryatwavelengthsfromcmtoopticalpenetratesdifferentdepthsinthestellarphotosphere. e-MERLIN,theEVLA andALMA willhavethesensitivityandtheimagingfidelitytoresolvethesuggestedlargeconvectioncellsinredsupergiantsandAGB starsouttoafewhundredpc(orfurtherforRSG).Byobservingatsuccessivelylowerfrequenciesatsuitabletimeintervals, wewilltestwhetherindependent(convective)orcorrelated(pulsation-driven)disturbancesdominate. Co-ordinatedVLBA ande-MERLINmaserobservationswillshowwhetherstarspotsdirectlyleadtoSiO maserclumpsandwhetherthesesurvivethedustformationprocess. WehopethatthiswillcomplementedbyVLTI,MROI orotheroptical/IR interferometrywhichwouldrevealtherelativedistributionofhotandalsoofabsorbingmaterialinthestronglyconvectivezone. Moreover, existingobservationsshowthatthestarsareasymmetric. Persistentaxisymmetrywouldsuggestthatanorderedmagneticfieldisimportant(intheabsenceofdetectablerotationforeffectivelysolitarystars)whilstvaryingdirectionswouldsuggestcomplexpulsationmodes.
ResolvingdebrisdiscsinterrestrialplanetregionswithMIDI-VLTI
RachelSmith (KeeleUniversity)with M.C. Wyatt(IoA UniversityofCambridge), and C.A. Haniff
(CavendishLaboratory, UniversityofCambridge)
DustinmostdebrisdiscsoriginatesinplanetesimalbeltsakintotheKuiperbeltat> 30AU fromtheirstars. Relativelyfewstarsexhibitdustat < 30AU.BecauseofthesmallspatialscalesinvolvedadirectdeterminationofthediscmorphologyinsuchregionsrequirestheuseoflongbaselineinterferometrywithinstrumentssuchasMIDI ontheVLTI.InthistalkwepresentMIDI observationsoffourdebrisdisctargetswithdustbelievedtolieintheterrestrialplanetregions(∼ 1AU).Theyouthoftwoofthesetargets(12-16Myr)meansthattheobserveddustcouldbeindicativeoftheon-goingformationofterrestrialplanets. Fortheremainingtwooldertargets(1.3-2Gyr)thedustislikelytobeindicativeofarecenttransientevent. WediscussthelimitswecanplaceonthediscstructurewiththeMIDIobservations, andhowtheselimitscanbeinterpretedwithindifferentmodelsforthedustorigin.
CharacterisingtheconvectionpatternonBetelgeuse
JohnYoung (UniversityofCambridge)withA. Chiavassa, X. Haubois, E. Pedretti, B. Plez,
E. Josselin, G. Perrin, and B. Freytag
TheredsupergiantBetelgeuse(AlphaOrionis)isanirregularvariablestar. Betelgeuseisthoughttoexhibitlarge-scaleconvectiveprocessesthatareimportantdriversofthevariabilityandmasslossfromthestar. Wereportnewmodellingofhigh-angularresolutionobservations, primarilyfromtheCOAST andIOTA interferometers, spanningseveralobservationepochsandmultiplewavebandswithintheI andH photometricbands.Theinterferometricobservables(visibilityamplitudesandclosurephases)arecomparedwithad-hocmodelsfortheapparentbrightnessdistributionandwith3D hydrodynamicsimulationsobtainedwithCO5BOLD,post-processedusingtheradiativetransfercodeOPTIM3D.Wefindthatthe3D simulationsareabletomatchtheobservedwavelength-dependenceoftheasymmetricbrightnessdistributionatallofthethreeepochstested,althoughtheapparentstellardiameterinbandpasseswithmoderateTiO opacityis5-10%largerthanpredictedbythesimulations. Hencewehaveconfirmedthepresenceofagranulationpatternfeaturingsmalltomediumscale(5–15mas)convection-relatedsurfacestructuresandalarge(∼ 30 mas)convectivecell.
P23A NanoflareDistributionGeneratedbyRepeated
RelaxationsTriggeredbyKinkInstabilityMichaelBareford (TheUniversityofManchester)
with Philippa Browning, andRonaldVander Linden
Itisthoughtlikelythatvastnumbersofnanoflaresoccurringinthesolaratmosphereareresponsibleforthecoronahavingatemperatureofmillionsofdegrees. WeproposethatsuchindividualheatingeventcanbetriggeredwhenacoronalloopbecomesunstabletoanidealMHD kinkmode. Afeatureofthemodelisthatitpredictsheatingeventswitharangeofsizes, dependingonwheretheinstabilitythresholdforlinearkinkmodesisencountered. Dissipationoftheloop'smagneticenergythroughfastmagneticreconnectionbeginsduringthenonlinearstageoftheinstability, whenlocalisedfragmentarycurrentsheetsform.
Theloopisrepresentedasastraightline-tiedcylinderwithzeronetcurrent. Thetwistinginducedbyrandomphotosphericmotionsarecapturedbytwoparameters, representingtheratioofcurrentdensitytofieldstrengthforspecificregionsoftheloop. Onsetofinstabilitycanthusbemappedasaclosedthresholdinthe2dimensionalparameterspace. Afterflaring, theloopevolvestothestateoflowestenergywheretheratioofcurrenttofieldisconstantandhelicityisconservedinaccordancewithRelaxationTheory. Weconsiderthattheloopundergoesrepeatedepisodesofinstabilityfollowedbyrelaxation, orthattheinstabilityandrelaxationtakesplaceinanensembleofsimilarloops; hence,afrequencydistributionofeventsizes(nanoflares)iscollated. Here, themodelisextendedtomuchmorerealisticconfigurationswhichcorrespondtolocalisedphotospherictwisting, andhencehavezeronetcurrent(contrastingwithpreviousworkinwhichtheloophadanetcurrent). Weshowthe
P22–P23 73
resultsobtainedfromusingtwomethodsofcurrentneutralisationthatarecompatiblewithanon-zeromagneticflux. Theseresultsarecomparedwiththoseoftheearlierstudy.
Comparisonofmodelsoffluxtransfereventformationusingpredictedandobserved
asymmetryRobertFear (UniversityofLeicester)with
Steve Milan, Joachim Raeder, and David Sibeck
Fluxtransferevents(FTEs)areburstsofmagneticreconnectionataplanetarymagnetopauseandhavebeenobservedatEarth, JupiterandMercury.Theyareusuallyidentifiedbybipolarsignaturesinthecomponentofthemagneticfieldnormaltothemagnetopause(Bn). SeveralconceptualmodelshavebeenproposedforFTE formation, includingmodelsbasedonreconnectionatasinglereconnectionline(X-line)andatmultipleX-lines.Two-dimensionalmagnetohydrodynamicmodelshavepreviouslybeenusedtosimulatebothscenariosandhavefoundatendencyforFTEsgeneratedbysingleX-linereconnectiontoexhibitanasymmetryintheBnsignature, withtheleadingpeakbeingsubstantiallysmallerinmagnitudethanthetrailingpeak. Ontheotherhand, FTEsimulationsfeaturingmultipleX-linereconnectionledtomoresymmetricsignatures. WepresentacomparisonofthesesimulationresultswithobservationsmadeattheEarth’smagnetopausebytheClusterspacecraft, usingadatasetof213FTEswhichwereobservedbyallfourspacecraftin2002/3. A tendencyisfoundfortheBnsignaturestobeasymmetric, butwiththeleadingpeakstrongerthanthetrailingpeak- oppositetothepredictionmadebythe2D models. Wealsocomparetheobservationswiththeresultsofamorerecentglobal3D MHD simulationandfindsimilartrendstothoseobservedbyCluster.
TurbulentrelaxationofbraidedmagneticfieldsGunnarHornig (UniversityofDundee)withAnthony Yeates, Antonia Wilmot-Smith, and
David Pontin
Magneticbraidingofcoronalloopsduetothemotionoftheirphotosphericfootpointshaslongbeendiscussedasapossiblemechanismfortheheatingofthesolarcorona(E.Parker, 1972). Thismotivatedaseriesofnumericalexperiments(Wilmot-Smithetal. 2009, 2010)ontheturbulentrelaxationofbraidedmagneticfields. TheseexperimentshaveproducedrelaxedstateswhichdifferdrasticallyfromthepredictionsoftheTaylorhypothesis.
Wepresentanewtopologicalmeasure, atypeofgeneralisedfluxfunction, whichallowsustoanalysetherelaxationprocessandwhichshowsthattherearefurtherconstraintsontherelaxationprocessbeyondtheconservationofthetotalhelicity, whichpreventthesystemfromrelaxingtoaTaylorstate.
3-D MagneticreconnectionatseparatorsClareParnell (UniversityofStAndrews)with
Andrew Haynes, and Rhona Maclean
Magneticseparatorsarespecialfieldlinesthatconnecttwomagneticnullpointsandlieontheintersectionofthesurfacesmadeupoffieldlinesthatextendfromthenullpoints. Three-dimensionalreconnectioncanoccurinmanylocationsincludingnullpoints, separatrixsurfacesandseparators. Weconsidertheimportanceofseparatorreconnectionbyconsideringvarious3DresistiveMHD experimentsinwhichreconnection
isakeyprocess. Inparticular, wediscussthefrequencyofoccurrenceofseparators, theirbehaviourandthenatureofreconnectioninthevicinityofaseparator. WewillconcludebyindicatingtheconsequencesofseparatorreconnectionfortheSun.
A surveyofHXR emissionofseismicallyactiveandquietX-classwhite-lightflares
EhsanPedram (UniversityCollegeLondon–MSSL)with Sarah Matthews
Sun-quakes, generatedduringtheimpulsivephaseofsomesolarflares, arethemostintenseacousticradiationobservedonthesolarsurfaceandofferinterestingpossibilitiesforfurtheringourunderstandingofflaresandactiveregionhelioseismology. Variousmechanismshavebeenproposedastohowseismicwavescanbegeneratedfromasolarflare. Recentworkhasshownaclosecorrelationbetweenenhancedcontinuumemissionandtheseismicemissionobservedduringtheimpulsivephase. InthisstudywehaveexaminedtheHXR emissionfromYohkohandRHESSI togetherwithwhitelightemissiondataobservedbyGONG andTRACE.Highrateofenergydepositionandtheareaoverwhichtheenergyisbeingdepositedonsuggestsback-warmingasaplausiblemechanismforgeneratingsun-quakes. Combiningthisresultwithspatialandtemporalcorrespondenceofwhite-lightemissionwiththepeakintensityofHXR emissionfurtherenhancesthispossibilitywhichisinagreementwithfindingsofpreviousstudies.
Regimesofmagneticreconnectionat3D nullpoints
DavidPontin (UniversityofDundee)withE.R. Priest, and K. Galsgaard
Magneticreconnectionat3D nullpoints-- aswellastheseparatrixandseparatorstructuresassociatedwiththem-- isthoughttobeofgreatimportanceintheSolarcorona. Ourunderstandingofthereconnectionprocessesthatmayhappenatnullshascomealongwayinrecentyears, althoughmanyopenquestionsremain.Recentadvancesintheoryandcomputationalexperimentshaveshowntheneedtorefinethepreviouscategorisationofmagneticreconnectionatsuch3D nulls. Wepresenthereanewcategorisationintothreebasicmodes, dependingonthenatureoftheflownearthespineandfanofthenull. Wewilldiscussthebasicpropertiesofthesethreereconnectionmodes- 'spinefanreconnection', 'torsionalspinereconnection'and'torsionalfanreconnection'. Particularemphasiswillbeplacedonthemostcommon'spine-fan'reconnectionmode, inwhichthenullpointlocallycollapsesformingacurrentsheetspanningboththespineandfan, andresultingintransportofmagneticfluxacrossboththefanandspine.
Doesmagnetichelicityeffectactiveregionevolutionandenergetics?
AlisonWallace (UniversityCollegeLondon–MSSL) with LucieM. Green, SarahA. Matthews,
Cristina Mandrini, Pascal Demoulin, andLidiavan Driel-Gesztelyi
ThepuposeofthisstudyistoinvestigatetheinteractionsbetweensameandoppositehelicitystructuresincludinglargescalereconnectioneventssuchasflaresandCMEs, aswellassmallscaleevents. Ofthesetwoscenarios, theonethatproducesthemostenergyisstillatopicfordebate.Wepresentobservationsoftwoactiveregionsfollowingtheemergenceofabipole, onewiththe
sameandonewiththeoppositesignofhelicityfromtheactiveregion. InbothcasesnewfluxemergedattheNorth-Westernedgewithinthenegative(leading)polarity. Thelifetimeofthefirstbipolewas37hrsandthecounter-helicitybipolewas67hrs. Wediscusstheroleofreconnectioninre-distributinghelicityandhowthiseffectstheactiveregionevolution.
Relaxationofbraidedcoronalloopsbymultiplesmall-scalereconnectionevents
AntoniaWilmot-Smith (UniversityofDundee)withDavidI. Pontin, Gunnar Hornig,
AnthonyR. Yeates, and Klaus Galsgaard
Braidingofthesolarcoronalmagneticfieldisaprimecandidateforcoronalheating. Wereassessmagneticbraidingwithparticularemphasisonrecentdevelopmentsin3D magneticreconnectiontheory, concentratingontheevolutionoftheintegratedparallelelectricfield, acrucialquantityfor3D reconnection.
Westartwitharealisticbraidednon-linearforce-freemagneticfieldwithzerototalmagnetichelicity. ThefieldisnotinresistiveMHDequilibriumandwetrackthelossofstabilityandsubsequentdynamicsviaanumericalsimulation.Strongcurrentconcentrationsareformedintheearlyevolution, thelocationofwhichisgovernedbyregionsofinitiallyhighintegratedparallelelectricfield.
Subsequentlythefieldundergoesaturbulentrelaxation, evolvingintotwounlinkedforce-freefluxtubes. Detailsofthereconnectionprocessesduringrelaxationareexamined; magneticfluxisfoundtoevolveinacomplexmannerandisreconnectedmultipletimes. TheendstateoftherelaxationsuggestsasegmentedTaylor-likeprocesstakesplaceandthatadditionalconstraintsbeyondtheconservationoftotalhelicitygoverntherelaxation. Someprogresstowardsdeterminingtheseconstraintsisreported.
PropertiesoftheDistributionFunctionofaVlasov-MaxwellEquilibriumfortheForce-Free
HarrisSheetFionaWilson (UniversityofStAndrews)with
Thomas Neukirch, and Michael Harrison
A discussionispresentedofaVlasov-Maxwellequilibriumrecentlydiscoveredfortheforce-freeHarrissheet. Fortheforce-freeHarrissheet, forcebalanceismaintainedbyamagneticshearfieldinsteadofagradientoftheplasmapressure, theplasmapressurebeingconstantalongwiththedensityandthemagnitudeofthemagneticfield.Thedistributionfunctionrecentlyfoundfortheforce-freeHarrissheethasanumberofinterestingproperties, whichvarywithparametervalues. Forexample, thedistributionfunctioncanbemulti-peakedintwoofthevelocitydirections, whichmayhaveimplicationsfortheonsetofmicro-instabilities.
3D MagneticNullpoints: LocalisedFantiltingandTorsionalReconnection
PeterWyper (Sheffield)with Rekha Jain
MagneticReconnection, aprocessofbreakingideal- MHD frozen-in-fluxconstraintsonfieldlineconnectivity, isbelievedtobeanefficientmechanismforheatingthesolarcorona. Theprocessisofgreatimportanceinmanyotherastrophysicalandlaboratoryplasmas. Themagneticfieldintheseplasmascanbeverycomplexwiththreedimensional(3D) structure.
74 P23
Reconnectionleadstoarearrangementofthemagnetictopologyandareleaseofstoredmagneticenergyinsuchstructuresifthefieldlinesaretwistedorsheared. Itcanalsoreleaseenergyandaccelerateparticleswherelargegradientsofthemagneticfielddevelop, forexamplemagneticnullpoints. Recenttheoreticalprogressinourphysicalunderstandingofthe3D nullpointreconnectionhasbeentoexaminemagneticfluxandplasmaflowsacrosstheFanandSpineandtounderstandtheirtimeevolution. Inthistalk, wewilldiscussthreetypesofsecondaryreconnectionarounda3D nullpointfromananalyticalstandpoint: Fantilting/distortion, TorsionalspineandTorsionalfan.
P24TheHeliophysicsIntegratedObservatory
RobertBentley (UniversityCollegeLondon–MSSL) with Mike Hapgood, Chris Perry,
John Brooke, AnjaLe Blanc, Kevin Benson, andVineeth Shetty
TheHeliophysicsIntegratedObservatory, HELIO,iscreatingacollaborativeenvironmentwherescientistscandiscover, understandandmodeltheconnectionbetweensolarphenomena,interplanetarydisturbancesandtheireffectsontheplanets. HELIO willprovideintegratedaccesstodatafromthesolar, heliospheric, geophysicsandplanetarydomainsandallowtheusertoundertakeasearchforinterestingeventsandphenomenabasedsolelyonmetadataanddataproducts.
WewilldescribehowHELIO canbeusedtoaddressscienceproblemsthatspanthedomainsbyallowingtheusertotrackphenomenaastheypropagatethroughthesolarsystem.
TheHELIO infrastructureisbeingdevelopedaroundaservice-orientedarchitecture. Thesearchforinterestingeventsandphenomena, andthetaskofthenfindingandretrievingthedatahasbeensplitintoanumberofservicesthatcaneitherbeusedindependentlyoraspartofaworkflow.
VersionsofsomeoftheHELIO servicesarestartingtobecomeavailableandwearelookingforuserthatcanhelptestandrefinetheseandassistinthetaskofdefininguserinterfacesthatbettermatchtheneedsoftheresearchcommunity.
HELIO isaresearchinfrastructurefundedunderCapacitiesprogrammeoftheEC's7thFrameworkProgramme(FP7); theprojectstartedinJune2009andhasadurationof36months. TheHELIOConsortiumincludesthirteengroupsfromtheUK,France, Ireland, Italy, Switzerland, SpainandtheUS.
A ComprehensiveStudyofthe13-15May2005SolarEvent(s)
MarioBisi (AberystwythUniversity)withA.R. Breen, B.V. Jackson, R.A. Fallows, A.P. Walsh,
M.J. Owens, Z. Miki, P. Riley, C.J. Owen,A. Gonzalez-Esparza, A.G. Wood, E. Aguilar-
Rodriguez, H. Morgan, E.A. Jensen, M. Tokumaru,P.K. Manoharan, K. Fujiki, I.V. Chashei,A.S. Giunta, J.A. Linker, V.I. Shishov,
S.A. Tyul’bashev, G. Agalya, S.K. Glubokova,P.P. Hick, J.M. Clover, B. Pintér, and A. Buffington
Wepresentanoverviewoftheresultsofamulti-technique, multi-instrument, co-ordinatedstudyofthesolar-eruptiveeventof13May2005anditsprogressionthroughtheinnerheliosphere. We
havecombinedobservationsandmeasurementsfromcoronalandinterplanetaryremote-sensinginstruments, interplanetaryandnear-Earthin-situmeasurements, remote-sensingobservationsandin-situmeasurementsoftheterrestrialmagnetosphereandionosphere, alongwithcoronalandheliosphericmodelling. WediscusstheresultantEarth-directed(halo)coronalmassejection(CME),andbriefly, theeffectsontheterrestrialspaceenvironmentandupperEarthatmosphere. Theseanalysesareusedtotracetheorigin, development, propagation, terrestrialimpact, andsubsequentconsequencesofthiseventtoobtainthemost-comprehensiveviewofageo-effectivesolareruptiontodate. FulldetailsofthestudyofthiseventcanbefoundinBisietal.,SolarPhysics, TopicalIssue(TI) onRemoteSensingoftheInnerHeliosphere, 2010, whentheTI ispublished.
AssessingtheaccuracyofCME speedandtrajectoryestimatesfromSTEREO observationsthroughacomparisonofindependentmethodsChristopherDavis (STFC RutherfordAppletonLaboratory)with J.A. Davies, and J. Kennedy
WehaveestimatedthespeedanddirectionofpropagationofanumberofCoronalMassEjections(CMEs)usingdatafromtheSTEREOHeliosphericImagers. Ingeneral, thesevaluesareingoodagreementwiththosepredictedbyThernisienetal(2009)usingaforwardmodellingmethodtofitCMEsintheSTEREO COR2coronagraphdata. ThereissomeevidencefromthissurveythatthespeedofaCME ismodulatedbytheambientsolarwindspeed. Thetechniquewasverifiedbyin-situdatawherepossible. WealsoshowthattheuncertaintiesinourderivedparametersareinfluencedbytherangeofelongationsoverwhicheachCME istracked. Inordertoreducetheuncertaintlyinthepredictedarrivalat1AU towithin6hours, aCME needstobetrackedouttoatleast30degreeselongation.SuchatechniqueallowsthepredictionofEarth-directedCMEstobemadelonginadvanceoftheirarrival, providingapotentialadvanceinspace-weatherforecasting.
PropagationofanEarth-DirectedCoronalMassEjectionin3D
PeterGallagher (TrinityCollegeDublin)withJasonP. Byrne, ShaneA. Maloney, and R.T. James
McAteer
Wehavedevelopedanewmethodtoreconstructthe3D evolutionofaCME frontusingtheSunEarthConnectionCoronalandHeliosphericInvestigation(SECCHI) onboardtheSolarTerrestrialRelationsObservatory(STEREO).On12December2008anEarth-directedCME wasobservedbySTEREO whilethespacecraftwereinnearquadratureat86.7ºseparation. ThispositioningpresentsanidealcaseforobservingitspropagationthroughthecombinedSECCHIinstrumentfields-of-viewandapplyingourtechniquetoreconstructtheCME frontin3D.ThereconstructionallowsustodeterminethetrueCME frontkinematicsandmorphology, andwemeasurethreeimportantdynamiceffectsatplay:deflectionfromahighlatitudesourceregion; anincreasingangularwidth; andinterplanetarydrag.
SolarStormwatch: acrowd-sourcingapproachtounderstandingCoronalMassEjections
MarekKukula (RoyalObservatoryGreenwich)withChris Davis, Chris Lintott, and Natasha Waterson
TheSolarStormwatchprojectisanewonlineinitiativewhichmakesuseofthelargearchiveofdatafromtheSTEREO missiontogainadeeperunderstandingoftheoriginandpropagationofCoronalMassEjections. SolarStormwatchispartofthenewwaveof“crowdsourcing”or“citizenscience”projectswhichenlistmembersofthepublictohelpcarryoutresearchwhichcouldnotbedonebyscientistsworkingalone. Thespacecraftdataarepresentedinanappealingandaccessiblewaywhichisheavilyinformedbythedesignofpopularonlinegames. Thewebsiteincludestutorialsectionswhichallowinteresteduserstofindoutmoreaboutsolarphysicsaswellasasectionforschoolswithsuggestionsforclassroomactivities. Howeverthesciencegoalsaregenuineandwillleadtousefulandsignificantresearchoutput. Aswellascarryingoutrigorousanalysisofanotherwiseunder-utiliseddataset,userscanparticipateinavibrantonlinecommunitywhichincludesscientistsfromtheSTEREO mission. ExperiencewithpreviouscitizenscienceprojectssuchasGalaxyZooshowsthatasignificantsubsetofuserswilleducatethemselvestothepointatwhichtheyareabletospotunusualphenomenaandbringthesetotheattentionofthescienceteam, raisingtheprospectofentirelyunexpectedandnoveldiscoveries. TheprojectisaninitiativeoftheRoyalObservatory, GreenwichinpartnershipwiththeRutherfordAppletonLaboratoryandtheCitizenScienceAlliance. Assuch, itharksbacktotheprominentrolewhichtheObservatoryplayedinsolarphysicsinthe19thandearly20thcenturies.
Probingtheevolutionofcoronalandheliosphericstructureswithsuprathermalelectrons
MathewOwens (UniversityofReading)withNancy Crooker, Nathan Schwadron, Tim Horbury,
Benoit Lavraud, and Alexis Rouillard
Thedistributionandevolutionofmagneticfluxatthephotosphereiscomplex. Itisdominatedbymid-latitudemagneticfluxemergence, whichsubsequentlymigratestothepoles, ultimatelyfacilitatingthesolarcyclepolarityreversal. Thisismorphologicallydifferenttothefieldreversalobservedintheheliosphere, whichproceedsasasimplerotationofanapproximatelydipolarfield.Themagnetically-dominatedcoronalinksthesetwodisparateregions, thoughtheprocessesresponsibleforthenecessarysolarcyclerestructuringofthecoronaarenotwellunderstood. Ithasbeensuggestedthatcoronalmassejections(CMEs)playacriticalroleincoronalreconfiguration, bysheddingexcesshelicity, addingfluxtotheheliosphereandtransportingopenfluxinthemannerrequiredforthesolarcyclepolarityreversal. Suprathermalelectronobservationsprovideameanstotesttheseideas. I’llpresentasummaryoftheseobservationsandattempttointerprettheminthewidercontext.
Investigatingtheobservationalsignaturesofmagneticcloudsub-structure
KimberleySteed (UniversityCollegeLondon–MSSL) with C.J. Owen, P. Demoulin, and S. Dasso
Magneticcloudsareasub-setofinterplanetarycoronalmassejections(ICMEs)thatexhibitamagneticfluxropestructure. Theyareoftenprimarilyidentifiedbysmooth, large-scalerotationofthemagneticfield, howeverbothsmalland
P24 75
large-scalefluctuationsofthemagneticfieldareobservedwithinsomemagneticclouds. Wehaveidentifiedasmallnumberofmagneticcloudswithinwhichmultiple, small-scalereversalsofthegradientoftheazimuthalmagneticfieldareobservedtowardstheircentres, andwehereinusetheterm'sub-structure'torefertotheregionsthatexhibitthissignature.
On13April2006, amagneticcloudwasobservedbyACE andWindwhichdisplaysmanyofthetypicalcharacteristicsusedtoidentifyamagneticcloud, andalsoexhibitstheclearestexampleofsub-structuretowardsitscentrethatwehavefound. Investigationsofthemagneticfieldobservationsthatcharacteriseamagneticcloudcontainingsub-structureandassociatedchangesintheplasmaobservationshaveshownthatthemagneticstructuredoesnotevolveoverashorttimescaleoftheorderofafewminutes, andthatthismagneticcloudissubjecttocompression,probablyasaresultofthefastsolarwindstreambehindit, whichisparticularlystronginthesub-structureregion. Wesuggestseveralpossibleexplanationsforsub-structurewithinmagneticclouds, includingthepresenceofmultiplefluxropes, warpingofthemagneticcloudstructureandinsitumagneticreconnection.
Smallscaletransientfeaturesatcoronalholeboundaries: apossiblesourcefortheslowsolar
wind?SrividyaSubramanian (ArmaghObservatory)with
M.S. Madjarska, and J.G. Doyle
Coronalholesareregionsofpredominantlyunipolarcoronalmagneticfieldswithasignificantcomponentofwhichisopenintotheheliosphere.Ouraimwastofurtherexplorethesmall-scaleevolutionofCH boundariesusinghigh-resolutionandhigh-cadenceimagesfromtheX-raytelescope/HinodetakenwithanAlPolyfilter. WeidentifiedtransientX-raybrighteningsinequatorialcoronalholes, polarcoronalholes, andthequietSunwithandwithouttransientcoronalholesusinganautomatedidentificationprocedure. WefoundthatincomparisontothequietSun, theboundariesofcoronalholesareabundantwithbrighteningeventsincludingareasinsidecoronalholeswhereclosedmagneticfieldstructuresarepresent. ThestatisticalinvestigationofX-raybrighteningsshowedthataround70%ofthemincoronalholesandtheirboundariesshowexpandingloopstructuresand/orcollimatedoutflows, whileonly30%inthequietSunshowoutflowswithmostofthemappeartobecontainedinthecoronabyclosedmagneticstructures. WesuggestthattheejectedplasmaguidedbytheopenmagneticfieldlinesincoronalholesandtheirboundariesescapestheSuncontributingtotheslowsolarwind.
CharacterisingtheSTEREO HeliosphericImagersignaturesofCorotatingInteractionRegions
AnthonyWilliams (UniversityofLeicester)withS.E. Milan, J.A. Davies, C.J. Davis, and
R.A. Harrison.
DuringthecourseoftheSTEREO missionveryfewcoronalmassejectionshavebeenobserved, evenfewerhavebeenobservedtobeEarth-directed.Despitethis, theHeliosphericImagers(HI) detectastampedeofoutward-propagatingcoronalplasmaenhancements, indicatingstructuredsolarwindoutflow. A widelyreportedmethodofestimatingthespeedanddirectionfromelongation-time(J-)mapsoftransienteventswhichallowsthepredictionofthetime-of-arrivalofthese
featuresatEarth. Whilethismethodisreportedtoworkwhencomparingtimesofarrival, itfrequentlyappearstoproducespeedsfarlowerthanthespeedswhentheyareeventuallydetectedbyin-situspacecraftsuchasACE.TobetterunderstandthenatureofthesesignaturesweinterpretfamiliesoftracesasoriginatingfromasinglecoronalholeboundaryonthesurfaceoftheSungivingrisetoacorotatinginteractionregion(CIR).WesuccessfullyshowacorrespondencewithassociatedCIR signaturesobservedatACE,anddissecttheanatomyofaCIR asseenbyHI.Theseresultshighlightthedifficultyofinterpreting2D imagesofthe3D heliosphere, whenthereareoftenwithmanysimultaneousactiveregionsandoverlappingheliosphericstructuresalonganyparticularline-of-sight. WeoutlinestrategiesforthefutureinterpretationofHI images.
Non-potentialenhancementoftheSun'sopenmagneticflux
AnthonyYeates (UniversityofDundee)withD.H. Mackay, and A.A. vanBallegooijen
Formingafundamentaldynamicalconnectionwiththeheliosphere, theSun'slarge-scalemagneticfieldisshapedbyinteractionsinthelowercorona(belowabout2.5solarradii).Traditionalmodelsfortheglobalmagneticstructureinthisregionhaveusedpotentialfieldsourcesurface(PFSS) extrapolationsfromphotosphericmagneticobservations. However, insituspacecraftmeasurementsoftheinterplanetarymagneticfieldoverseveralsolarcyclesshowthatthePFSS extrapolationspredicttoolowalevelofopenmagneticfluxduringepochsofhighersolaractivity. Herewesuggestthatthisdiscrepancymayberesolvedbyrelaxingthepotential-fieldassumptionandallowingforelectriccurrentsinthelowcorona. Wedemonstratetheconceptusingaquasi-staticnumericalmodelofthelarge-scalecoronalmagneticevolution, whichsystematicallyproducesthesecurrentsthroughfluxemergenceandshearingbysurfacemotions.Thecurrentsinflatethemagneticfield, enhancingtheopenfluxduringperiodsofhighersolaractivity, inagreementwithIMF observations. Inaddition, theejectionofmagneticfluxropesinthemodelmimicstheeffectofcoronalmassejectionsthatcauseshort-termfluctuationsintheheliosphericmagneticfield.
Arethereimprintsofhotplasmaoutflowsfromactiveregionsinthesolarwind?
LidiavanDriel-Gesztelyi (UniversityCollegeLondon–MSSL) with A.N. Fazakerley, and
L.K. Harra
HinodehasdiscoveredapotentialsourceofsolarwindattheedgesofactiveregionswithXRT andEIS (e.gSakaoetal., 2007, Harraetal., 2008,Doscheketal., 2008). Theseoutflowsarelong-lastingandexistattheedgesofmostactiveregions. WehaveexaminedinterplanetarysolarwinddatafromtheACE spacecraftandsolarremotesensingdataincludingEIS plasmaupflows,duringafullCarringtonRotationinterval. WediscusswhethertheevidencesupportstheideathattheflowsthatweseeonthesurfaceoftheSunactuallyaretransportedtotheEarthinthesolarwind, orifitsuggeststhattheyaremerelyrelatedtoflowsinlarge-scaleloops.
P25FindingtheSourceofUHECRsusingBayesian
AnalysisofPierreAugerDataLauraWatson (ImperialCollege, London)with
Andrew Jaffe, Daniel Mortlock, and Roberto Trotta
Cosmicraysareextremelyenergeticparticlesandmustoriginatefromsomeofthemostenergeticprocessesinnature. DeterminingtheirorigincouldshedlightonprocessesthatplayakeypartintheUniverse'sevolution. Itissuspectedthatultrahighenergycosmicrays(UHECRs)maycomefromactivegalacticnuclei(AGNs): statisticalanalysesofthecorrelationbetweenthelocationofAGNsandUHECR detectionsweremadepossibleforthefirsttimebyobservationsfromthePierreAugerobservatory(PierreAugerCollaboration,Science318, 938, 2007). However, whilstthesefindingshinttowardscorrelation, amorerecentanalysishasfoundaweakenedcorrelation(Nature463, 1011, 2010). Herewepresentacompletelydifferentapproachtotheproblemwhichtakesthefullamountofavailableinformationintoaccount.ThroughBayesiananalysis, weprovideamethodforfindingtheprobabilitythatUHECRsoriginatefromAGNsanddiscusstheextensionofthismethodtothecomparisonofdifferentsources.
P26Globalpopulationstatistics, bimodalityand
multivariatedistributionsofgalaxieswithSDSS.IvanBaldry (LiverpoolJMU)
TheSDSS increasedthenumberof z < 0.2
galaxieswithknownredshifts, spectralandmulti-colourmeasurements, byanunprecedentedfactoroverthecourseofafewyears. Thishasledtoanexplosioninstudiesoftheglobalpopulationstatisticsofgalaxies. Thedangerintheseanalysesisthatimportantdetailsarelost, ontheotherhand, theycanprovidestrongconstraintsongalaxyevolutionandtheyprovideadescriptionofourUniverseonatrulycosmicscale. I willreviewsomeoftheSDSS resultsobtainedusingglobalpopulationstatisticsincludingthesignificantcolourbimodalityandenvironmentaltrends.
Whitedwarfsastracersofstellar, binary, andplanetaryevolution
BorisGaensicke (UniversityofWarwick)
I willreviewthetremendousimpactthattheSloanDigitalSkySurveyhashadonourunderstandingofawidevarietyofastrophysicalenvironmentscontainingwhitedwarfs. Besidesincreasingthetotalnumberofknownwhitedwarfsmorethanfive-fold, allowingdetailedstudiesoftheirgalacticpopulation, SDSS hasfoundnew, rarebreedsofwhitedwarfsthattraceextremebranchesofstellarevolution. SDSS hasalsoprobedthepopulationsofaccretinganddetachedwhitedwarfbinariestoanunprecedentedlevelofdetail, providingthemoststringenttestsofbinaryevolutiontodate. Atotallyunexpecteddiscoverywastheidentificationofplanetarydebrisdiscsaroundwhitedwarfs,originatingfromthetidaldisruptionofrockyasteroids. Assuch, thesesystemsofferaglimpseintothedistantfutureofourownSolarsystem,and, moregenerally, provideinsightintothelateevolutionofplanetarysystems.
76 P24–P26
EvidenceofTidalStrippingofthreecompactelliptical(cE) galaxiesdiscoveredinSDSS DR7
AvonHuxor (UniversityofBristol)withS. Phillipps, J. Price, and R. Harniman
Wepresentthreecompactgalaxies, foundinasearchofSDSS DR7, whichexhibitclearevidenceoftidalsteams. Thegalaxiesarelowmass, andhavesmalleffectiveradii, andtheirspectraindicatethattheypossessyoungtointermediate-agestellarpopulations. TheseprovidedirectevidencefortheprocessoftidalstrippingthatisbelievedtobetheoriginofM32-typegalaxies, a"smokinggun". Thesecompactgalaxiesareallfoundinsmallgroups, suggestingthatwemaybeseeingtheformationofsuchgalaxiesindynamicallyyounggalaxygroupings. OneofthethreeisfoundinasmallgroupnotunliketheLocalGroupitself, andthusprovidesanadditionalmodelforunderstandingM32.
GalaxyClusteringintheSDSSJonLoveday (UniversityofSussex)
I willreviewwhatwehavelearntaboutgalaxyclusteringfromtheSDSS,includingconstraintsontheHaloOccupationDistribution(HOD)formalism, therelativeclusteringofgalaxiesofvaryingcolourandluminosity, andthefirstandsubsequentdetectionsoftheBaryonAcousticPeakinthegalaxydistribution.
DVORAC Detector- TheDurhamVOronoiRed-sequenceAutomatedClusterDetectorfornext-
generationpanoramicsurveysDavidMurphy (DurhamUniversity)with
Jim Geach, and Richard Bower
WepresenttheDVORAC detector, anewclusterdetectionalgorithmdesignedforlargepanoramicsurveyswithmulti-bandphotometry. Themethodmakesnopriorassumptionsonthepropertiesofclustersotherthan(a)thesimilarityincolourofclustergalaxies(theredsequence)and(b)alargeprojectedsurfacedensity. Thedetectorhastwomainstages. First, itidentifiesclustermembersbyphotometricallyfilteringtheinputcataloguetodetectover-densitiesincolour-magnitudespace.Second, aVoronoitessellationidentifiesregionsofhighsurfacedensityandgroupsgalaxiesintoclusters. Asthenextgenerationofsurveysprobetofainterlimits, quickandefficientalgorithmswillberequiredtohandlethevastvolumesofdatagenerated. ToprepareforthePanoramicSurveyTelescopeandRapidResponseSystem(PanSTARRS) survey, wehavetestedthedetectorontheSDSS Equatorial"Stripe82", andamockMediumDeepSurvey(MDS) PanSTARRScataloguebasedonthe ΛCDM modelwithasemi-analyticgalaxyformationrecipe. WewillshowthatclustersdetectedintheSDSS showgoodagreementwithexistingclustercataloguesandthatthebenefitofdeeperdatahasallowedustoidentifymanypreviouslyundetectedclustersandgroups. Themocksurveyhasallowedustoquantifytheefficiency, robustnessandreliabilityofthealgorithmbycomparingthecatalogueofdetectedclusterstothemembershipofgalaxiesindarkmatterhaloes.
AnalysingtheClusteringofPhotometricallySelectedGalaxies
AshleyRoss (UniversityofPortsmouth)withWillJ Percival, and RobertJ. Brunner
TheSDSS hasproducedphotometricredshiftcatalogswhichcontainover20milliongalaxies.Wehavecreatedofapproximatelyvolumelimited
samplesofthesegalaxies, allowingprecisemeasurementsoftheangular2-pointcorrelationfunctionofgalaxies. Splittingthesegalaxiesintoredshiftshellsbetweenz=0.1and0.4, wehavefoundasignificantincreaseinthebiasof L*galaxiesbetweenz=0.1and0.4. Usingthemeasurementstodeterminethethehalo-occupation-distribution(HOD) ofthegalaxiesineachredshiftshell, wefindourmeasurementscanbeexplainedbytheformationof L*galaxiesinhalosofmass ∼ 1012h−1M⊙. Whenwesplitthegalaxiesbytype, wefindthat, inordertoself-consistentlyfitthemeasurements, early- andlate-typegalaxiesmustpreferentiallyexistinseparatedarkmatterhalos.
TheSDSS-III BaryonOscillationSpectroscopicSurvey(BOSS):FirstResults
NicholasRoss (LawrenceBerkeleyLab)withErinS. Sheldon, AdamD. Myers,
Christophe Yeche, and SDSS-III:BOSS Team
TheSDSS-III (www.sdss3.org)BaryonOscillationSpectroscopicSurvey(BOSS) isanewfive-yearproject, whichcommencedoperationsinlate2009. ThekeygoalsofBOSS aretomeasureredshiftsfor1.4millionLuminousRedGalaxies(LRGs)to z < 0.8, andsimultaneously160,000quasarsat z > 2.2. Bothsampleswillmeasuretheequationofstateofdarkenergyto1%usingtheBaryonAcousticOscillation(BAO) technique.HerewedescribethesomeoftheveryearlyresultsfromtheBOSS CommissioningPhasewhichtookplacein2009andearly2010.
Higher-OrderClusteringOfLuminousRedGalaxiesInTheSDSS
CristianoSabiu (None)with Robert Nichol, andFelipe Marin
TheSloanDigitalSkySurvey(SDSS) LuminousRedGalaxy(LRG) spectroscopicsampleprovidesuswithamapoflarge-scaleover- densitiesintheUniversewithinavolumeof ∼ 1 (Gpc/h)3. ThemainadvantageofusingLRGsisthattheyarehighlybiasedwithrespecttotheunderlyingdarkmatterandthusefficienttracersofthelarge-scalestructuresintheUniverse, e.g., LRGshavebeenessentialforthedetectionandmeasurementoftheBaryonAcousticOscillations(BAO).TomakefulluseoftheLRG samples, itisimportanttoaccuratelymodelthemappingbetweengalaxiesandthedarkmatter. Recently, thishasbeenachievedusingthe"halomodel"forhowgalaxiesinhabittheirdarkmatterhalos. Indetail, weusetheHaloOccupationDistribution(HOD) topopulateasuiteofN-bodysimulations(tocreateagridofmockcatalogues), andcomparethesetotheobservedLRG population. Toaddconstrainingpower, weusetheThree-PointCorrelationFunction(3PCF),whichencodesmuchmoreinformationthantheusualtwo-pointstatistics. Inthistalk, wepresentresultsofourHOD analysisforanLRG sampleselectedfromthefinalDR7SDSS catalogue.
SDSS-II SNe- AnOverviewandHostGalaxyProperties
MathewSmith (UCT) with R. Nichol, H. Lampeitl,B. Dilday, B. Bassett, and SDSS-II SNeSurvey
Team
MeasurementsoftypeIaSupernovaehaverevolutionisedthecosmologicalmodelthroughtheintroductionofDarkEnergy. TheSDSS-IISupernovaSurveyspectroscopicallyidentifiedover500oftheseeventsatintermediateredshift(0.05 < z < 0.5)andobtainedhighqualitylight-
curvesforhundredsmore. BycombiningtheseSNeIa'swiththosefromothersurveys, themostaccuratemeasurementsofthecontentoftheUniversehavebeenmade. Weshalldescribethesurveyitself, it'sdeterminationofthecosmologicalparametersandinvestigatetherelationshipthatthesecosmologicalprobeshavewiththeirlocalenvironment. BycreatingarobustandrepresentativesampleofSNeIa'swehaveshownthattheseeventsarefarmorelikelytoappearingalaxieswithrecentstar-formationactivitythan"passive"galaxies, andthattheSNeIarateisstronglydependentonhostgalaxystar-formationrate. Additionally, weshowthatthereisanenvironmentdependenceofthestretchdistributionsoftheseevents, andintriguinglythatSNeindifferentenvironmentsmaypossessdifferentabsolutemagnitudesanddifferentdustlaws.
DiscoveryofthefirstwideL dwarf+giantbinarysystemandeightotherultra-cooldwarfsinwide
binariesZengHuaZhang (UniversityofHertfordshire)withDavid Pinfield, Avril Day-Jones, Ben Burningham,
and Hugh Jones
Weidentify806ultra-cooldwarfsfromtheirSDSSrizphotometry(ofwhich34arenewlydiscoveredL dwarfs)andobtainpropermotionsthroughcrossmatchingwithUKIDSS and2MASS.Propermotionanddistanceconstraintsshowthatnineofourultra-cooldwarfsaremembersofwidelyseparatedbinarysystems; SDSS 0101(K5V+M9.5V),SDSS 0207(M1.5V+L3V),SDSS0832(K3III+L3.5V),SDSS 0858(M4V+L0V),SDSS0953(M4V+M9.5V),SDSS 0956(M2V+M9V),SDSS 1304(M4.5V+L0V),SDSS 1631(M5.5V+M8V),SDSS 1638(M4V+L0V).Oneofthese(SDSS 0832)isshowntobeacompaniontothebrightK3giantEtaCancri. Suchprimariescanprovideageandmetallicityconstraintsforanycompanionobjects, yieldingexcellentbenchmarkobjects. EtaCancriAB isthefirstwideultra-cooldwarf+giantbinarysystemidentified. WepresentnewobservationsandanalysisthatconstrainthemetallicityofEtaCancriA tobenearsolar, anduserecentevolutionarymodelstoconstraintheageofthegianttobe2.2- 6.1Gyr. IfEtaCancriBisasingleobject, weestimateitsphysicalattributestobe: Mass = 63 − 82MJup,Teff = 1800 ± 150 K, log g = 5.3 − 5.5,[M/H] = 0.0 ± 0.1. Itscoloursarenontypicalwhencomparedtootherultra-cooldwarfs, andwealsoassessthepossibilitythatEtaCancriB isitselfanunresolvedbinary, showingthatthecombinedlightofanL4+T4systemcouldprovideareasonableexplanationforitscolours.
BinarypopulationsinSDSS:A newdiagnosticforsystemparametersofevolvedwhitedwarf
binariesLiekevanSpaandonk (UniversityofWarwick)with
D. Steeghs, and T.R Marsh
EvolvedbinarysystemsformalargesubsetofbinarystarsandCataclysmicVariables(CVs)areavaluablesamplewithinthisgroupastheyprovidehomogeneousconfigurationsofwhitedwarfsplusnearmain-sequencemassdonors. A keyexpectationbasedonourcurrentunderstandingofbinaryevolutionisthatangularmomentumlossdrivesCVstoshortorbitalperiodsastheirmassdonorstarsshedmass. Theyprovidethesettingforthestudyofaccretionontocompactobjects,includingTypeIasupernovaeandgravitationalwaveemission. However, theseshort-period
P26 77
systemsarefaintandthereforesampleshavetraditionallybeenbiasedagainstthem.
ThishasfinallychangedthankstoCV searcheswithinSDSS astheyareunearthingshort-periodsystemsinlargernumbers. Althoughtheorbitalperiodisanimportantdiagnostic, reliablemassestimates(e.g. massratio q = Mdonor/MWD)areneededforthedonorstarstoplaceaCV onitsevolutionarytrack.
Wehavestudiedpromisingcandidatesatthebrightendoftheshort-periodbinarysample,exploitingtheCaII tripletlinesinordertorecovertheirbinaryparameters. TheCaII linesofferadvantagesoverthehydrogenandheliumlinescommonlyused, asthelatteraredominatedbybroadaccretiondiscprofiles. Ourdatasofarclearlyvindicatethisstrategy, asmostsystemsrevealsharpemissionfromtheintrinsicallyfaintdonorsontopofthediscemission, allowingustodeterminethebinaryparametersinsystemssuchasrevealedbySDSS.
P27TheLastMajorEpochofDiskGrowthinM33MichaelBarker (RoyalObservatoryEdinburgh)with A. Ferguson, R. Ibata, M. Irwin, G. Lewis,
T. Smecker-Hane, and N. Tanvir
Late-typediskgalaxieslikeM33arecommoninthenearbyuniverse, butdifficulttoproduceincosmologicalsimulations, soabetterobservationaldeterminationoftheirevolutioniscrucialforunderstandingdiskformation. Tothatend, weuseHubbleSpaceTelescopeAdvancedCameraforSurveysimagingtostudythestarformationhistory(SFH) oftwofieldsat9.1and11.6kpcalongM33’snorthernmajoraxis. Basedonthedistributionofstarsinthecolour-magnitudediagrams, wefindthatthemajorityofstarsinbothfieldsformedat z < 1. Themeanageoftheinnerfieldis ∼ 3 Gyrandthemeanageoftheouterfieldis ∼ 6 Gyr. TheseresultsofferthemostdetailedviewyetofM33’speripheryandprovideamuch-neededobservationalconstraintonthelastmajorepochofdiskassemblyinthisgalaxy.
BPASS:BinaryPopulationandSpectralSynthesisJohnEldridge (InstituteofAstronomy(Cambridge))
with Elizabeth Stanway, Norbert Langer,Monica Relano, and Christopher Tout
Thereisgrowingobservationalevidencethatthebinaryfractionofmassivestarsisclosetounity.Thereforetomodelyoungstellarpopulationsaccuratelythecomplexandnon-linearevolutionofbinariesmustbeincluded. Wehavecreatedapowerfulanduniquebinarypopulationandspectralsynthesiscode, BPASS,thataccountsforbinaryevolutionbyusingthousandsofdetailedbinarystarmodelsincreatingsyntheticstellarpopulation(Eldridge&Stanway, 2009,MNRAS,400, 1019). Wediscusstheimportantdifferencesthatwefindbetweensinglestarandbinarypopulationsforvariedobservablesofresolvedandunresolvedstellarpopulations. Wealsoshowhowthesedifferencesgrowasthemetallicityofthestellarpopulationdecrease.
DependingontimewewillalsodiscoverhowwearetestingandcalibratingBPASS bystudyingsystemssuchasNGC604inM33thatareresolvedbyHST butunresolvedbyothertelescopessothatwecanhavegreaterconfidenceinBPASS when
applyingittostudyingthestellarpopulationsofhigh-redshiftgalaxies.
ConstrainingtheInitialMassFunctionIgnacioFerreras (UniversityCollegeLondon–
MSSL) with Dominik Leier(ARI,Heidelberg), andPrasenjit Saha(Zurich)
TheInitialStellarMassFunction(IMF) remainsoneofthemainunknownsinsyntheticmodelsofstellarpopulations. ThemassiveendoftheIMFcanbeconstrainedviastudiesofopenclustersandyoungpopulations. However, thelow-massendoftheIMF ismuchhardertoconstrainduetothelowluminosityofstarsbelow1Msun. AlternativemethodsestimatingthetotalmassareneededtosetconstraintsonthelowerendoftheIMF.InthistalkI willpresentrecentworkfocusedontheEinsteinCross. A non-parametricanalysisofthelensingsystemiscomparedwithpopulationsynthesismodels. A combinationofhighresolutionimagingwithHST/NICMOS anddeepspectroscopywithVLT/FORS givesM/L predictionsthatarecomparedwithanumberofpopulationsynthesismodelsforarangeofIMFs. I willalsopresentpromisingnewmethodsbasedonmulti-variateanalysistoconstraintheIMF fromspectroscopicdataofunresolvedstellarpopulations.
KinematicbiasinexoplanetsurveysRichardHutcheon (KeeleUniversity)with
P.F.L. Maxted
Over400exoplanetsarenowknown, discoveredmainlybythetransitorradialvelocitymethods.FromthesesystemsweselectaBrightTransitSample(BTS) andaRadialVelocitySample(RVS).Duetoobservationalconstraintsthedistancesofstarsinthesesampleslieinalmostnon-overlappinggroups, furtherorcloserthan100pcfortheBTS andRVS respectively. Sincethetransitsurveysavoidlowgalacticlatitudes, theBTS starstendtoliefurtherfromtheGalacticplane. Wehaveinvestigatedwhetherthesebiasesareexpectedtointroducedifferencesinthedistributionofageormetallicity, parameterswhicharethoughttoinfluencethefrequencyofexoplanets.
TheaverageandmedianmetallicitiesoftheRVSarerespectively0.03and0.10dexhigherthanfortheBTS.Calibrationsamplesofsolar-typestarswithsimilarkinematicstotheBTS andRVS starshavebeenpreparedandtheseshowamedianmetallicity0.02dexhigherfortheRVS.Thecalibrationsamplesarelargeenoughtorevealevensmalldifferencesbetweenthem. Henceanydifferenceinmetallicitiesisverysmallandisduetokinematics. Themetallicitiesoftheactualsamplesareabout0.2dexhigherthanforthecalibrationsamples; thisconfirmsearlierresultsthatplanethoststarsaremetal-richcomparedwithothersolar-typestars. ThereisnosignificantdifferencebetweentheagesofthestarsintheBTSandRVS samplesortheircalibrationsamples, butthisismostlyduetothelargeuncertaintyinestimatingtheagesofmain-sequencesolartypestars.
Weconcludethattheselectioneffectsinherentinthetransitsurveyandradialvelocitytechniquescan, inprinciple, leadtodifferentbiasesinthemetallicityandagedistributionsofthestarsobservedbutthisdifferenceappearstobenegligibleinpractice.
Crystallinesilicatesaroundoxygen-richAsymptoticGiantBranchStarsintheLarge
MagellanicCloudOliviaJones (UniversityofManchester)with
F. Kemper, B.A. Sargent, G.C. Sloan, P.M. Woods,A.K. Speck, M. Matsuura, J.-P. Bernard,
K.D. Gordon, R. Indebetouw, K.E. Kraemer,E. Lagadec, J. Th. vanLoon, I. McDonald,
M. Marengo, M. Meixner, W.T. Reach, andA.G.G.M. Tielens
Ithasbeenshownthatthesilicatesinthedustshellsaroundoxygen-richstarsontheasymptoticgiantbranch(AGB) canshowaconsiderabledegreeofcrystallinity. A thresholdvalueforthemass-lossrateexists, abovewhichthefeaturesduetothecrystallinesilicatesforsteriteandenstatiteappear. Weareinvestigatingtheoriginofthisthresholdvaluebyexpandingthecrystallinitystudiestothemetal-poorenvironmentoftheLargeMagellanicCloud(LMC).WepresentSAGE-SpecSpitzer-IRS spectroscopyforanumberofO-richAGB starsintheLMC.The5-40micronspectraoftheseevolvedO-richobjectsencompassarangeofspectralfeaturesandbandstrengths; fromthespectrallyrichwhichexhibitawealthofcrystallineandamorphoussilicatefeaturestothe`naked'(dust-free)stars, acrossarangeofmass-lossrates,providinganidealopportunitytoexploretheonsetofcrystallinity. Wemeasuredthefeaturestrengthofcrystallinesilicatebandsat23.6, 28, 33.6 µm,withrespecttothestrengthofthecontinuumproducedbythermalemissionfromamorphoussilicates. WeintendtoplotthesevaluesagainstMdust and Mgas, inordertosearchforacorrelationwiththedustandgasdensityrespectively. TheserelationsmaybedifferentattheLMC'smetallicityof ∼ 0.5 Z⊙. WecompareourresultstothoseforO-richAGB starsintheGalaxy.
Theroleofminormergersinthestarformationhistoryofearly-typegalaxies
SugataKaviraj (ImperialCollegeLondon)withRichard Ellis, Sukyoung Yi, Kevin Schawinski,
Joseph Silk, GALEX Collaboration, and MUSYCCollaboration
Anexcitingrecentdiscoveryhasbeenthedetectionofwidespreadrecentstarformation(RSF) innearbyearly-typegalaxies(ETGs), usingnewsurveydataintherest-frameUV.Wereviewthecurrentstatusofthiswork, withaparticularemphasisonthedriversofthisstarformation.DatafromtheGALEX UV survey(z < 0.1),combinedwithdeepopticalsurveys(e.g. MUSYC,GOODS,COSMOS) thattracetherest-frameUVathighredshift, indicatethatETGsofallluminositiesformstarsoverthelifetimeoftheUniverse, withluminoussystems(−23 < MV < −21)formingupto10-15%oftheirstellarmassafterz=1. WhilesmallmassfractionsofyoungstarsseemtobeubiquitousinthenearbyETG population, thesourceofthisstarformationremainsamatterofdebate. WedemonstratethattheRSF atlateepochscannotbedrivensolelybyinternalmassloss, suggestingthatsomeormostofthegasfuellingtheRSF isexternallyaccreted. VisualinspectionofHSTimagesofETGsfromtheCOSMOS surveyatz∼ 0.5 showaremarkablecorrespondencebetweenthepresenceofmorphologicaldisturbancesandUV excess, whichsuggeststhatmergersmaybetheprincipaldriverofthisRSF.However, themajormergerrateisfoundtobetoolowtosatisfythenumberofETGsthatcarrysuchmorphologicaldisturbances, suggestingminormergersastheprimarychannelofgasaccretionandstarformationintheETG population. We
78 P27
discusstheimplicationsofrepeatedminormergeractivityonthespectralanddynamicalevolutionofmassivegalaxiesanddrawcomparisonswiththeliteraturewhichsuggestthatminormerging, ahithertopoorlyexploredprocess, maybeakeyelementoftheevolutionofgalaxiesatlateepochs.
Systematicuncertaintiesinherentinstellarpopulationsynthesismodelsandtheirimpacton
integratedspectraofstellarpopulations: Amodeller'sperspective.
SusanPercival (LiverpoolJohnMooresUniversity)
Stellarpopulationsynthesismodelsareavitaltoolforinterpretingthepropertiesofstellarpopulations(age, metallicity, SFH) inbothstellarclustersandgalaxies. ErrorsonthesederivedpropertiescanstemfromsystematicuncertaintiesintheSPSmodelsthemselves, and/orfromcertainpropertiesinherentinthestellarpopulationwhichcancomplicatetheinterpretationofresults. Allstellarpopulationsynthethismodelsrelyoncalibrationsofthe3mainstellarparameters- effectivetemperature, surfacegravityand[Fe/H].Thesescalesareimplicitinstellarmodels, isochronesandsyntheticspectra, andareexplicitlyadoptedforempiricalspectrallibraries. InthistalkI willdiscusstheeffectofamismatchinscalesbetweenisochronesandspectrallibraries(thetwokeycomponentsofSPS models)anddemonstratetheimpactongalaxyagesandabundanceratiosderivedfromcommonlyuseddiagnosticlineindices, andfromfullSED fitting. I willalsobrieflydiscusstheeffectofextendedbluehorizontalbranchesandstatisticalfluctuationsonthederivedpropertiesofstellarclusters.
TheAGB populationandthemetallicitygradientinNGC 6822
LisetteSibbons (UniversityofHertfordshire)withMaria-Rosa Cioni
NGC 6822isasmallIrregulardwarfthatformspartofthelocalgroup. Itscloseproximity(∼ 470
kpc)andapparentisolationprovideauniqueopportunitytostudygalacticevolutionwithoutstrongdynamicalfactors. ThisprojectaimstostudythemetallicitygradientandthedistributionofthestellarpopulationwithinNGC 6822viatheasymptoticbranchstar(AGB) componentofthestellarpopulation. Usingdeephighqualitynear-infraredphotometry, takenusingUKIRT in2008,thecarbon- andoxygen-richintermediate-ageAGB starshavebeenisolated. Theratiobetweenthesepopulations, theC/M ratio, hasthenbeenusedtoderivethe[Fe/H] abundancewithinthegalaxy. The[Fe/H] abundanceandthedistributionoftheAGB populationwerethenanalysedasafunctionofgalacticradius. Usingcolour-magnitudediagramsthetipoftheredgiantbranchstarshasbeenlocatedatKs=17.29±0.03andthecolourseparationforC- andM-typestarsfallsatJ-K =1.188±0.01. UsingthesecutsearlyresultsindicateanoverallC/M numberratioof0.248,withvariationinthenorthandsouth, aswellasatlargergalactocentricdistances. AlsoadenserAGBpopulationhasbeenlocatedintheSW regionofthegalaxyinthedirectionoftheouterspheroid.Summarizing, theresolvedAGB populationacrossthewholeofNGC 6822hasbeeninvestigatedandregionsofvaryingmetallicity, andAGB stellardensity, havebeenidentifiedwhichmayindicateachangeorsomepasteventinthestarformationhistoryofthegalaxy.
Learningaboutstellarpopulationsinunresolvedgalaxies
RussellSmith (DurhamUniversity)
I willreviewcurrenttechniquesforlearningaboutthestellarcontentofunresolvedgalaxies, throughintegrated-lightspectroscopy. Thesemethodshavebecomeacrucialweaponintheobservationalastronomer'sarsenal, andarenowroutinelyappliedtosamplesrangingfromtensuptotens-of-thousandsofgalaxies, toconstrainthehistoryofstarformationandchemicalenrichmentinthedistantpast. Buthowdoweproperlyinterprettheresultsofsuchstudies? Howdowemakemeaningfulcomparisonstogalaxyformationmodels? Whathavewereallylearned? Whatarethecurrentlimitations, andaretheyfundamentalormerelypracticaldifficultiestoovercomewithlargertelescopesandcleverermodelling? I willelaborateonsomeofthesequestions, tostimulatediscussion, buttheycannotbeansweredinafifteen-minutetalk!
AGB StarsinWLMBejaminTatton (UniversityofHertfordshire)with
Maria-Rosa Cioni
Theaimofthisprojectistoinvestigatethestarformationhistoryandmetallicityofthelocalgroup, irregulardwarfgalaxyWLM (Wolf-Lundmark-Melotte).
ThemaindatausedforthisstudyiswidefieldJHKsnearinfraredimagingspanningaregionofapproximately1sq. degreeobtainedwiththeWideFieldCameraonUKIRT.
Colour-magnitudediagrams(J-KsvsKs)allowedforthedeterminationofthetipoftheredgiantbranchandfortheidentificationC-typeandM-typestarslocations. TheC/M ratiowasthencalculatedleadingtotheproductionofasurfacemapofmetallicitydistribution. Theseresultswerecomparedwithinformationintheliterature.
ThestellarpopulationsintheLargeMagellanicCloud
PaulWoods (UniversityofManchester)withSAGE-Specteam
I presenttheclassificationresultsofSAGE-Spectroscopy, aSpitzerLegacyprojectwhichobtainedIRS spectraofanumberofpoint-source-likeobjectsintheLargeMagellanicCloud(LMC).SuchasurveygivesusinformationaboutthedustcontentoftheLMC,andidentifyingthenatureoftheobjectsdetectedinthemid-IR helpsustounderstandhowthatdustiscycled. I willdetailtheobjectclassificationprocess, andtheresultswhichcanbedrawnfromsuchanendeavour. Wecanreliablydistinguishredsupergiantsfromoxygen-richAGB starsbymeansofcolour, andareabletotracetheevolutionofcarbon-richevolvedstarsbymeansoftheirdustcontent. Wealsofindthat(massive)youngstellarobjectsfallintooneoffourevolutionarygroupings.
P28Thedriftofauroralradioabsorptionpatches
observedbyimagingriometerJohnHargreaves (UniversityofLancaster)with
M.J. Birch, and B.J.I. Bromage
Thephenomenonofdriftingpatchesofauroralabsorption, firstrecognisedinthe1960s, ishere
illustratedinrecentobservationswithanimagingriometerinnorthernFinland. Possiblecausesareconsidered, usingincoherent-scatterobservationsfromEISCAT andF-regionvelocitiesfromSuperDARN.
MagneticfieldparallelcurrentsintheUCL-CTIPmodel
TimothySpain (UCL) with RichardB. Horne, andAlan Aylward
ThemagneticfieldparallelcurrentsintheEarth'sionospheredonotcontributetoeithertheiondragorJouleheatingofthethermosphere, duetothecross-productbetweenthetotalcurrentandthemagneticfieldintheseterms. Asaresult, thecalculationofthesecurrentswasneverexplicitlyincludedintheUCL-CTIP model, despitetheperpendicularcomponentsofthecurrentbeingcalculatedinaself-consistentmanner. Thecalculationofthefieldparallelcurrentcomponentallows, forexample, thecalculationofthetotalmagneticfieldbythepoloidal-toroidalmethod.HerewepresentamethodofcalculationofthefieldparallelcomponentofthetotalcurrentandanapplicationofthiscalculationtosomesimpleexperimentsperformedwiththeUCL-CTIP model.
ModellingGeomagneticallyInducedCurrentsintheNationalGridusingSAMNET.
KatieTurnbull (LancasterUniversity)withA.W.P. Thomson, C. Beggan, J.A. Wild, and
F. Honary
WepresentthefirstresultsofanewmodelwhichusesmagnetometerdatatocalculateGeomagneticallyInducedCurrents(GIC)throughouttheUK NationalGrid. GIC arearesultofrapidvariationsinthegeomagneticfield, suchasthoseobservedduringmagneticstormsandsubstorms. GIC cantravelalongpowertransmissionlinesasquasi-directcurrent,potentiallydamagingtransformersandresultinginblackouts.
ThenewUK modelusesSubAuroralMagnetometerNetwork(SAMNET) data, themethodofsphericalelementarycurrentsystemsona2D gridanda3D conductivitymodeloftheUK anditscontinentalshelftodeterminethesurfaceelectricfieldduringstorms. ThiselectricfieldisthenusedtocalculateGIC throughtheNationalGrid, throughthegroundingpointsofeachhighvoltagetransformerinthenetwork. WecomparemodelledGIC withmeasuredGIC duringoneparticularsubstormforfoursitesinScotland,aswellasdiscussingthemodelledGIC atsiteselsewhereintheNationalGrid. Infutureworkwewillexaminethegridresponseduringmajormagneticstorms, suchasthe'Halloween'eventofOctober2003.
P29A newenthalpy-basedapproachtothetransition
regioninanimpulsively-heatedcoronaPeterCargill (ImperialCollege)with
Steve Bradshaw
Observationsofthesolarcoronarevealpersistentandubiquitousred-shifts, whichcorrespondtobulkdown-flows. Foranimpulsively-heatedcorona(e.g. bynanoflares)thisindicatesthatamajorityofthecomponentloopstructuresareintheradiativelycoolingphaseoftheirlifecycle.However, thenatureofthebulkdownflowsraises
P27–P29 79
thepossibilitythatenthalpymayplayakeyroleintheenergybalanceoftheloopsandinparticularthatitpowersthetransitionregionradiation. Weuseonedimensionalhydrodynamicsimulationsofloopcoolingtoshowthatenthalpylossesfromthecoronaareeasilysufficienttopowerthetransitionregionradiation. Thiscontrastswiththelong-heldviewthatdownwardthermalconductionpowersthetransitionregion. Thetraditionaldistinctionbetweenthetransitionregionandthecoronaintermsoftemperaturealoneisthenagrosslyunphysicalsimplificationandaproperdefinitionoftheinterfacebetweentheseatmosphericlayersrequiresadetailedknowledgeoftheirenergybalance. Tothisendweproposearobustnewdefinitionofthetransitionregion.
Chromosphericmagneticreconnection:implicationsforjet-likeeventsandcoronal
heatingJiaoyangDing (ArmaghObservatory)withM.S. Madjarska, J.G. Doyle, and Q.M. Lu
Magneticreconnectioninthelowatmosphere,e.g., chromosphere, isinvestigatedinvariousphysicalenvironments. Itisfoundthatthetemperatureandvelocityoftheoutflowjetsasaresultofmagneticreconnectionarestronglydependentonthephysicalenvironments, e.g. themagnitudeofthemagneticfieldstrengthandtheplasmadensity. Thestrongermagneticfieldstrengthorthelowermassdensityis, theoutflowjetswithhighertemperatureandlargervelocityareobtained. Undercertainphysicalconditions,theoutflowjetscanbeheatedupto 2 × 106 K(coronaltemperatures), anditsmaximumvelocityreaches300- 400km/s. Inthiscase, bothcoldchromosphericjetsandhotcoronaljetsareobtainedsimultaneously. Thisisveryhelpfultounderstandtherelationshipbetweencoldandhotjets, aswellascoronalheatingmechanisms.
Observationand3D modellingofacoronalbrightpoint
ZhenghuaHuang (ArmaghObservatory)withM.S. Madjarska, K. Galsgaard, and J.G. Doyle
Weusemulti-wavelengthobservationsobtainedwithEIS,XRT andSOT onboardHinodetostudytheplasmapropertiesanddynamicsofacoronalbrightpointobservedinanequatorialcoronalhole. Theevolutionofthebrightpointwasfollowedinspectrallineswithformationtemperaturesfrom 104 K to 2 × 106 K,i.e. fromchromospherictocoronaltemperatures. Wefoundthatthebrightpointhasalongerlifetimeasseeninlowerchromospherictemperaturesthaninhigher,coronalones. WederivedthedensityevolutionofthebrightpointusingthespectrallineratioFeXII186/195. Weobtaineddensitieswhichfluctuateintherangefrom 8 × 108 to 3 × 109 cm−3 withanaverageofabout 2 × 109 cm−3. ThetimesequenceofXRT imagestakenwiththeAlpolyfilterwerealsousedtostudythedynamicsofthebrightpoint. Theplasmapropertiesofthebrightpointwillbecomparedwiththeoutputfroma3DMHD simulation. The3D modelisacombinationofastratifiedhydrostaticmodelatmosphereandapotentialmagneticfieldthatisobtainedusingpotentialmagneticfieldextrapolationfromlongitudinalmagnetogramfromSOT observations.ThemagneticstructureisstressedbyimposingaphotosphericvelocityflowderivedfrombluecontinuumSOT datausingballtracking.
CalculationandapplicationofR-matrixelectron-impactexcitationdataforionsofinterestto
astrophysicaldiagnosticmodellingGuiyunLiang (UniversityofStrathclyde)with
N.R. Badnell
A largenumberofhigh-resolutionandhigh-qualityspectrahavebeen, andcontinuetobe,obtainedfromboththeEUV (e.g. Hinode)andX-ray(e.g. Chandra, XMM-Newton, IXO) regions.Manyemissionlinesobservedinthesespectraarepotentialdiagnosticsoftheelectrontemperatureanddensityofcoronal-likehotplasmas. Therearealsomanyunidentifiedemissionlinesandlargediscrepanciesinlineintensityratioslikelyduetounknowncontaminants. Suchdiagnosticsandassociatedlineidentificationsrequireaccurateatomicdata, especiallyforelectron-impactexcitation.
Theadvantagesoftheintermediate-couplingframetransformationR-matrixmethod(Griffinetal.1998)makeitfeasibletoprovideexcitationdataalongK- andL-shelliso-electronicsequencescoveringasubstantialrangeofastrophysicallyimportantionsatthehigh-levelofaccuracyaffordedbythe R-matrixmethod. ThisisoneofthekeygoalsoftheUK AtomicProcessesforastrophysicalPlasmas(APAP) network. HerewewilladdresseffectivecollisionstrengthsalongtheNe-likeiso-electronicsequence(Liang&Badnell2010). Wealsolookataparticularion-Fe13+
(Liangetal. 2010)forwhichalaboratorymeasurementhasbeenmade. Weassesstheaccuracyofourexcitationdatainbothcases.
Usingthelatest R-matrixelectron-impactexcitationdata, weanalyzetheEUV andsoftX-rayspectraofhotplasmas, e.g. stellarcoronaandelectron-beamion-traps. SeveralpreviousquestionablelineintensityratiosinFe13+ havebeenexplainedsatisfactorilyandsomelinesareidentifiedinastrophysicalsourcesforthefirsttimewiththeaidofalaboratorymeasurementperformedattheHeidelbergEBIT (Liangetal.2010).
PlasmapropertiesofanX-rayjetfrommulti-instrumentco-observations: SUMER/SoHO,
EIS/XRT/HinodeandEUVI/SECCHI/STEREO AandB
MariaMadjarska (ArmaghObservatory)
Wewillpresentuniquemulti-instrumentobservationsofanX-rayjet-likeeventtakenwithSUMER/SoHO,EIS/XRT/HInodeandEUVI/SECCHI/STEREO.Thephenomenonaroseinacoronalbrightpointsituatedattheboundariesofanequatorialcoronalhole. Thecombinationoftwospectrometerscoveringtogetherthetemperaturerangefrom10000K to12MK andthethreeviewpointsofXRT,EUVI A andBpermittedustoderivetheplasmapropertiesanddynamicsofthisfeature. Weanalysedthebehaviourofdifferentspectrallinesduringthemicro-flaringwhichtriggeredthejet-likeevent.Wealsoobtainedthetemperaturesanddensitiesinthereconnectionsiteandthesurroundingregion.Thejetdynamicsanditsplasmapropertieswillbediscussedindetail. Wewillgiveoursuggestionsforthefutureinstrumentation(spectroscopicandimaging)andatomiccalculations.
AlfvénIonisationintheSolarPhotosphereProchetaMallik (UniversityofGlasgow)with
DeclanA. Diver, Lyndsay Fletcher, HughE. Potts,and CraigS. MacLachlan
Strongphotosphericflowsnearactiveregionsinevitablyinvolvemixingneutralgasand
magnetisedplasma. Wheretherelativespeedbetweenneutralandplasmaspeciesexceedsacriticalvalueatwhichtheenergyintheflowisequaltothefirstionisationpotentialofacomponentspecies, thatspecieswillbeionised.Thephysicalmechanismisasfollows: theneutralgasimpingingontheplasmacollideswiththepositiveionsanddisplacesthem, causingpocketsofnegativechargeimbalance. Theresultingelectricfieldsaccelerateatailofelectronstoenergiesabovetheionisationthresholdforparticulargasspecies. Thesenewionsremaintrappedinthemagneticstructure, leadingtoenhancedabundanceinthelowersolaratmosphere. Wepresentnumericalsimulationsoftheevolutionoftheelectrondistributioninsuchasituation, showinghowafractionoftheaffectedpopulationreachesenergiesabovetheionisationthresholdforparticularelements. Thisismostrelevantforlowcriticalionisationvelocity(CIV)elementssuchasXe, K,Cr, Mn, Feetc, andisakeydriverofelementover-abundance.
Non-LinearForce-FreeModeloftheSolarMagneticCarpet
KarenMeyer (UniversityofStAndrews)withD.H. Mackay, and A.A. vanBallegooijen
WemodelthedynamicalevolutionoftheSun'smagneticcarpet, andconstructanon-linearforce-freecoronalfieldbasedonsurfacemotions.Ratherthanindependentlyextrapolatingthecoronalfieldateachtimestep, wemodelacontinuousevolutionofthefieldthroughamagnetofrictionalrelaxationtechnique. Sofarwehavestudiedenergybuildupwithinthefieldduetothebasicinteractionsofcancellation,emergenceandflyby. ThemagnetofrictionalcodehasalsobeendirectlyappliedtoHinode/SOTmagnetogramdatatostudythelocationandvariationoflowcoronalnullpoints.
Detailedobservationsandmodellingofasmallflare
UrmilaMitraKraev (UniversityofCambridge(DAMTP)) with G. DelZanna, H. Mason,
S.J. Bradshaw, and A. Asai
Wehaveobtainedaplethoraofspatially- andtemporally-resolvedspectraldataofaB-classflarewiththeEIS spectrometeron-boardtheHinodesatellite. TogetherwithdatafromtheotherHinodeinstruments, aswellasGOES,TRACE andtheNobeyamaRadioHeliograph, adetailedpictureoftheevolutionofthisflareisputtogether. Theflareshowsmany'typical'featuressuchasprecursorevents, brighteningsintheribbons, andhot(10MK) emissionandsubsequentcooling. However,anumberoffeaturesarenew, suchasstrongblue-wingasymmetriesonlyseeninlinesformedbetween1.5and2.2MK.ThetemporalandtemperaturecoverageoftheEIS observationsprovidesnewinsightsintoourunderstandingofchromosphericevaporationandcooling. AnumericalsimulationusingtheHYDRAD codetostudythecoolingofthe10MK plasmaisingoodagreementwiththeobservations. Lineblendinginsomepotentiallyusefullinesforflarediagnosticsisalsodiscussed.
Theopticaldepthofwhite-lightflarecontinuumHughPotts (UniversityofGlasgow)with
Hugh Hudson, Lyndsay Fletcher, and Declan Diver
Thewhite-lightcontinuumemissionofasolarflareremainsapuzzleasregardsitsheightofformationanditsemissionmechanism. Thiscontinuum, anditsextensionintothenearUV,containthebulkof
80 P29
theenergyradiatedbyaflare, andsoitsexplanationisahighpriority. Wedescribeamethodtodeterminetheopticaldepthoftheemittinglayerandapplyittothewell-studiedflareof2002July15, makinguseoftheMDI intensityimages. Theopticaldepthofthevisiblecontinuuminthisflareissmall, consistentwiththeobservationofBalmerandPaschenedgesinotherevents.
Whatblinkersactuallyare?SrividyaSubramanian (ArmaghObservatory)with
M.S. Madjarska, J.G. Doyle, and D. Bewsher
Weinvestigateblinkersinanequatorialcoronalholeregionusingspectral, imagingandmagnetogramco-observationstofindoutwhattheseblinkersactuallyrepresent. WeusedanautomatedidentificationproceduretoidentifyblinkersinSoHO/CDS O v629Angstromrasters.WealsoidentifiedbrighteningsinSTEREO/EUVIFeIX 171AngstromimagesandHinode/XRT Alpolyimagestostudyblinkersatlowercoronaltemperaturesandtofindtheirpossiblecoronalcounterparts, respectively. AllCDS blinkershadEUVI 171Å counterparts. Identifiedblinkereventswereclassifiedintotwogroups, blinkerswithcoronalcounterparts, mostlyassociatedwithcoronalX-rayjets, andblinkerswithnocoronalcounterpartswhichappearaspointedbrighteningsattransitionregiontemperatures. Thelattercouldbesignatureofchromosphericfeatures(spiculesor/andmacrospicules)reachingtransitionregiontemperaturesorsimplyrepresentinducedflowsalongsmallscaleloopstructures. WebelievethatblinkersaretransientEUV responseofvariousdynamiceventsoriginatinganywhereinthesolaratmospherewhichcontributetothetemperatureraiseinthetransitionregion.
TheHydrodynamicEvolutionofImpulsivelyHeatedCoronalLoops: ExplicitAnalytical
ApproximationsDavidTsiklauri (QueenMaryUniversityof
London)with M.J. Aschwanden
Wederivesimpleanalyticalapproximations(inexplicitform)forthehydrodynamicevolutionoftheelectrontemperature T (s, t) andelectrondensity n(s, t), forone-dimensionalcoronalloopsthataresubjecttoimpulsiveheatingwithsubsequentcooling. Ouranalyticalapproximationsarederivedfromfirstprinciples,using(1)thehydrodynamicenergybalanceequation, (2)theloopscalinglawsofRosner-Tucker-VaianaandSerio, (3)theNeuperteffect,and(4)theJakimiecrelationship. Wecompareouranalyticalapproximationswith56numericalcasesoftime-dependenthydrodynamicsimulationsfromaparametricstudyofTsiklaurietal., coveringalargeparameterspaceofheatingrates, heatingtimescales, heatingscaleheights, looplengths, forbothfootpointandapexheating, mostlyapplicabletoflareconditions. Theaveragedeviationsfromtheaveragetemperatureanddensityvaluesaretypically ∼ 20%forouranalyticalexpressions.Theanalyticalapproximationsinexplicitformprovideanefficienttooltomimictime-dependenthydrodynamicsimulations, tomodelobservedsoftX-raysandextreme-ultravioletlightcurvesofheatedandcoolingloopsinthesolarcoronaandinflaresbyforwardfitting, tomodelmicroflares, toinferthecoronalheatingfunctionfromlightcurvesofmulti-wavelengthobservations, andtoprovidephysicalmodelsofdifferentialemissionmeasuredistributionsforsolarandstellarflares,coronae, andirradiance. M.J.Aschwanden, D.
Tsiklauri, Astrophys. J.Suppl. Ser., 185, 171-185(2009)DOI:10.1088/0067-0049/185/1/171
SpiculesandCoronalHeatingKamalamVanninathan (ArmaghObservatory)with
Maria Madjarska, and J.G. Doyle
Weusemulti-instrumentobservationsofspicules,lookingforevidenceofwhetherthesechromosphericfeaturescanalsobedetectedatcoronaltemperatures. WeanalysedCaII H imagesfromSOT/Hinode, comparingthemwithdatafromEIS/Hinode, plushigh-resolutiondatafromSUMER/SoHO.WeobservespiculesattheNorthpolewith10secondcadenceSOT data. A groupofrotatingspiculesasseenwithSOT areobservedintheSUMER transitionregionO V 629andN V1238asamacrospicule. EIS datadonotshowcorrespondingfeaturesatcoronaltemperatures.
MagneticreconnectionalongQSLs- amajordriverofactiveregionoutflows
LidiavanDriel-Gesztelyi (UniversityCollegeLondon–MSSL) with D. Baker, C.H. Mandrini,
and P. Demoulin
Therelationshipbetweenquasi-separatrixlayers(QSLs), orinthelimitofinfinitelythinQSLs,separatrices, andvariousactivityphenomenahasbeenexploredinmanydifferentsolarmagneticconfigurationsacrossallscalesinrecentyears. Intheabsenceofmagneticnulls, fastreconnectionalongQSLs, whicharespecificlocationsinthemagnetictopologywherefieldlinesdisplaystronggradientsofmagneticconnectivity, wasidentifiedasthemainphysicalprocessattheoriginofflares.Recently, itwasshownthatfast(tensofkm/s)persistenthotplasmaupflowsinactiveregions(ARs)canalsobelinkedtolocationsofQSLs. ItislikelythattheseupflowsthatoccurattheedgesofARsoverunipolarmagneticfieldconcentrationsareacceleratedbymagneticreconnectionalongQSLs. Wewillshowmulti-temperaturespectralscanobservationsfromHinode’sEIS combinedwithmagneticmodelingofQSLsintwoARsobservedon20-21February2007and11January2008. ThelatterAR isobservedandmodeledwhenitisinthevicinityofthesolarcentralmeridianwheretherearenoprojectioneffects,therebyeliminatingambiguitylinkingtheoriginofmulti-temperatureobservationsofAR upflowstoQSLs. WeusethePotentialSourceSurfaceModeltolookforopenfieldlinesinthevicinityofupflowsandQSL locationsinordertodemonstratewhethertheseupflowsbecomeoutflowsandcancontributetothesolarwind.
P30TheEffelsbergNorthernSkyPulsarSurvey
EwanBarr (MPIfR Bonn)
Pulsarsarerapidlyrotatingneutronstarswhichemitbeamsofbroadbandradioemissionfromtheirmagneticpoles. Theextremeconditionsfoundinandaroundpulsarsmakethemafantasticnaturallaboratorythroughwhichmanyaspectsoffundamentalphysicsandastronomycanbeprobed. Assuch, modernpulsarsurveysprovidethemeansthroughwhichwepavethewayfornewandexcitingscience. Whetheritisanexoticpulsarwhichpushesthelimitsoftheequation-of-state, ahighlyaccuratelytimingmillisecondpulsar(MSP) thatcanbeusedaspartofanarraytodetectgravitationalwavesoranormalpulsarthatwill
helpmaptheinterstellarmedium, thediscoveryofnewpulsarsinevitablyleadstoanimprovementinourunderstandingofoneormoreresearchareas.Thuswewillcommenceanorthernskyblindpulsarsurveywiththe100-mEffelsbergradiotelescopecomplimentedbyatwinsearchofthesouthernskywiththe64-mParkestelescope.
AlsopresentedhereisPSR J1745+1017,Effelsberg'sfirstevermillisecondpulsardetection,the18thradioFermipulsarsofardiscovered.
SurfaceextractionofelectronsinapulsarDeclanDiver (UniversityofGlasgow)with A.A. daCosta, E.W. Laing, C.R. Stark, and L.F.A. Teodoro
Wepresentanoveldescriptionofhowenergeticelectronsmaybeejectedfromthepulsarinteriorintotheatmosphere, basedonthecollectiveelectrostaticoscillationsofinteriorelectronsconfinedtomoveparalleltothemagneticfield.Thesizeoftheinteriormagneticfieldinfluencestheinteriorplasmafrequency, viatheassociatedmatterdensitycompression. Theplasmaoscillationsoccurclosetotheregionsofmaximummagneticfieldcurvature, thatis, closetothemagneticpoleswherethemajorityofmagneticfluxemerges. Giventhattheseoscillationshaveadensity-dependentmaximumamplitudebeforewave-breakingoccurs, suchwavescanejectenergeticelectronsusingonlytheself-fieldoftheelectronpopulationintheinterior. Moreover,photonsemittedbyelectronsinthebulkoftheoscillationcanescapealongthefieldlinesbyvirtueoftheloweropacitythere(andthefactthattheyareemittedpredominantlyinthisdirection),leadingtofeaturesinthespectraofpulsars.
GlitchesintherotationofPulsarsCristobalEspinoza (JodrellBankCentrefor
Astrophysics)with A.G. Lyne
A newsearchforglitcheswasperformedusingtheJodrellBankpulsartimingdatabase, and104newglitcheswerefoundintherotationof64pulsars.Combiningthesewiththosealreadypublishedwehaveputtogetheradatabasecontaining315glitchesin102pulsars. Thedatabasewasusedtostudytheglitchactivityamongthepulsarpopulation, findingthatitpeaksforpulsarswithacharacteristicage τ ∼ 10 kyranddecreasesforlongervaluesof τ , disappearingforobjectswithτ > 20Myr. Althoughtoalesserextent, theglitchactivityisalsolowerintheveryyoungpulsars(τ ∼ 1 kyr). Thecumulativeeffectofglitches, orthecolectionofmanyspin-upevents, actsagainsttheregularlong-termspindownrateofpulsars.Thepercentageofthespindownreversedbyglitchactivitywasfoundtovarybetween0.5%and1.6%forpulsarswithaspindownratebetween10−14 and 3.2 × 10−11 Hzs−1, decreasingtolessthan0.01%towardsbothhigherandlowerspindownrates. Theseratiosareinterpretedintermsoftheamountofsuperfluidinvolvedinthegenerationofglitches. Inthiscontext, theactivityoftheCrabpulsarmaybeexplainedbyquake-likeactivityonitscrust. Pulsarswithlowspindownratesseemtoexhibitmostlysmallglitches,matchingwellthedecreaseoftheamountofsuperfluidrelatedtoglitchactivity.
TheanalysisofglitchsizesindicatesthattheparticularglitchingbehaviourofPSR J0537-6910andtheVelapulsarmaybesharedbymostVela-likepulsars. Mostglitchesintheseobjectspresentthelargestfrequencyandfrequencyderivativejumpsrecorded, andseemtooccuratregularintervalsoftime.
P29–P30 81
A betterunderstandingoftheglitchingbehaviourofpulsarswillconductustowardsamorerefinedknowledgeofnotonlytheirinteriorsbutalsooftheirspinevolutionandgravitationalwaveemission.
Testsofgeneralrelativityandbinaryevolutionstudiesusingpulsarobservations
RobertFerdman (UniversityofManchester)
A briefreviewwillbegivenofseveralpredictionsofgeneralrelativity(GR) thatcanandhavebeentestedthroughtimingobservationsofpulsarsinbinarysystems. Thiswillcover, forexample,settinglimitsondipolargravitationalradiationandongravitationalconstantvariation, aswellasstrong-fieldtests. Alsotobediscussed, iftimepermits, isthestudyofbinarysystemevolutionusingpulsarobservations.
A BayesianSearchForGravitationalWaveRing-downsAssociatedWithPulsarGlitches
IkSiongHeng (UniversityofGlasgow)withJames Clark, Graham Woan, and Matthew Pitkin
Glitchesinpulsartimingarethoughttobeassociatedwithsuddenchangesinthepulsar'sangularmomentum. A fractionoftheexcessrotationalenergyisthenradiatedawayasgravitationalwaveemission. Wepresentasearchfordamped-sinusoidalgravitationalwaveringdownsusingBayesianmodelselection. Wedemonstratehowtheresultfromsuchasearchiseasilyconvertedintoastatementaboutthephysicalpropertiesofthegravitationalwaveemission.
CarbonatmosphereneutronstarinCassiopeiaA:YoungestneutronstarintheGalaxy
WynnHo (UniversityofSouthampton)withCraigO. Heinke
Thesurfaceofhotneutronstarsiscoveredbyathinatmosphere. Ifthereisaccretionafterneutronstarformation, theatmospherecouldbecomposedoflightelements(H orHe); ifnoaccretiontakesplaceorifthermonuclearreactionsoccurafteraccretion, heavyelements(e.g., Fe)areexpected. Despitedetailedsearches, observationshavebeenunabletoconfirmtheatmosphericcompositionofisolatedneutronstars. HerewereportananalysisofChandraobservationsoftheX-raysourceinthecentreoftheCassiopeiaAsupernovaremnant. Weshowthatacarbonatmosphereneutronstarproducesagoodfittothespectrum. Ouremissionmodel, incontrastwithothers, impliesanemissionsizeconsistentwiththeoreticalpredictionsfortheradiusofneutronstars. Thisresultsuggeststhatthereisnuclearburninginthesurfacelayersandalsoidentifiesthecompactsourceastheyoungest-known(withanageofabout330years)neutronstarintheGalaxy.
LatestHESS observationsofPulsarWindNebulaeDominicKeogh (DurhamUniversity)with HESS
Collaboration
Theconfinementoftherelativisticoutflowsofpulsarsproducesaluminouspulsarwindnebula(PWN) seenacrosstheelectromagneticspectrum.ThesesourcesareoneofthemostprominentclassesobservedbyTeV CherenkovobservatoriessuchastheNamibianbasedHESS telescopes.NumerousPWN havebeenobservedwithHESS,whileadditionaldarksourcesmayrepresentrelicPWN.InthistalkI shalloutlinesomeofthemostexcitingrecentobservationsofpulsarwindnebulaewiththeHESS telescopes.
TheopticalandinfraredcounterpartofSGR0501+4516
AndrewLevan (UniversityofWarwick)
I willpresentthediscoveryoftheoptical/IRcounterparttothesoft γ−repeaterSGR0501+4516. Unlikethemajorityofmagnetars,thisoneliesinthegalacticanticentredirection,andhasonlymoderateextinction, allowingustosearchforitscounterpartatlongerwavelengths.Ourcomprehensivecampaignofobservationsbeganonlyanhourafterthefirstactivationofthesource, andcontinuedfor14months. TheseobservationsrevealseveralcrucialdiagnosticsoftheIR counterpartofanSGR i)rapidoptical/IRvariabilityshowsaperiodalmostidenticaltotheX-rayderivedperiod(5.7s), ii)Thelongtermoptical/IR variationappearstotrackthatintheX-rayiii)Limitsonthepropermotionsuggestthatthespatialvelocityis < 400 km/s, andshowthatSGR0501+4516isnotassociatedwithanysupernovaremnants, oryoungstellarclusters, afirstforamagnetar.
Knownpulsarsascontinuousgravitationalwavesources
MatthewPitkin (UniversityofGlasgow)
Knownpulsarsareapotentialsourceofcontinuousgravitationalwavesandtherehavebeenongoingsearchesforthemwithincurrentgravitationalwavedetectordata. Nosignalshaveyetbeenseen, butbasedontheexpectedsensitivitiesoffuturedetectorsweexaminethepotentialfordetectingthem. Weexaminewhatkindofstar(e.g. strangequarkstar, hyperonstar,ornormalneutronstar)theseobjectswouldhavetobetoachievedetection. Wealsostudywhatdetectionscouldinferaboutthestrainonthestar'scrust.
TheeffectofGravitationalDistortionofSpacetimeonPulsarTiming
SatoruSakai (UniversityofGlasgow)withGraham Woan, and MartinA. Hendry
Theaimofthisresearchistodeterminetheimpactofgravitationallensingonpulsartiming, anditsimplicationsforthedetectionofgravitationalwaves. Gravitationallensingoccurswhenamassivebodypassesclosetotheline-of-sightbetweentheEarthandasource. FromGeneralRelativity, thiscausesspace-timedistortionswhichresultinanextrapathlengththatthelightmusttravel, andsubsequentlyadelayinthetimeofarrival. Thisresearchwilllookattherateofchangeof(gravitational)Shapirotimedelay.
IntermittentRadioEmissionfromPSR B0823+26NeilYoung (UniversityofManchester)with
M. Kramer, A. Lyne, B. Stappers, and P. Weltevrede
Intermittentpulsarsarecharacterisedbyperiods,uptoyears, whentheirradioemissionisofffollowedbysimilarlylongperiodswhentheyareon. Theyofferauniqueinsightintomagnetosphericphysicsofpulsars. PSR B0823+26isacandidateofthispulsarclass. IntensiveobservationsofthissourcewerecarriedoutwiththeLovellTelescope, atJodrellBank, fromJanuarytoJune2009. Thispulsarhassubsequentlybeenfoundtoexhibitquasi-periodicradioemissionphases, ontimescalesshorterthanthatobservedinthecanonicalintermittentpulsarB1931+24. Here,I presenttheresultsandanalysisoftheseobservations.
PulsarElectrodynamics: TheRelativisticKineticTheoryofRadiativePlasmas—TheGamma-ray
cut-offAntonioArmandodaCosta (InstitutoSuperior
Técnico, Lisboa, Portugal)with D.A. Diver,E.W. Laing, C.R. Stark, and L.F.A. Teodoro
Theclassicalmodellingofradiationbyacceleratedchargedparticlesinpulsarspredictsacut-offinphotonenergyataround25GeV.Whilstthisisbroadlyconsistentwithobservations, theclassicaltreatmentisnotself-consistent, andcannotbeextendedtoexplaintherarehigh-energydetectionsofphotonsinthe100sofGeV range. Inthispaperwerevisitthetheoreticalmodellingofhigh-energyradiationprocessesinverystrongelectromagneticfields, inthecontextofbothsingleparticlesandcollectiveplasmas, whichimpliesanextensionoftheVlasovtheoryofcollisionlessplasmas, totakeintoaccountradiativeprocesses. Therearenoclassicalconstraintsonthisdescription. Wefindthatthereisindeedacriticalenergyofaround50GeV thatarisesnaturallyinthisself-consistenttreatment,butratherthanbeingacut-off, thiscriticalenergysignalsatransitionfromradiationthatisclassicaltoaquasi-quantumdescription, inwhichtheparticleisabletoradiatealmostitstotalenergyinasingleevent. Thisnewmodellingthereforeplacespulsarradiationprocessesonamoresecurephysicalbasis, andadmitsthepossibilityoftheproductionofTeV photonsinaself-consistentway.
P31TheCo-EvolutionofMassiveGalaxiesandtheir
SupermassiveBlackHolesoverthelast11.5GyrsAsaBluck (UniversityofNottingham)with
Christopher Conselice, Omar Almaini, Elise Laird,Kirpal Nandra, and Mark Dickinson
Supermassiveblackholes(SMBHs)arenowthoughttobeaubiquitousconstituentofmassivegalaxies. Despitetheirrelativelysmallcontributiontothemassofgalaxies(< 1/1000)theyexertapowerfulinfluenceovertheirevolution–possiblytriggeringstarformationandbeingultimatelyresponsibleforshuttingthisstarformationoff. TightrelationshipsarefoundtoexistinthelocalUniversebetweenglobalpropertiesofhostgalaxies(suchasluminosity, stellarmassandvelocitydispersion)andthemassofthecentralSMBH.ThissuggestsacausalconnectionbetweengalaxiesandSMBHs, thenatureofwhichisstillpoorlyunderstood. I willintroducemyapproachtoinvestigatethiscausalconnectionthroughprobingtheredshiftevolutioninthe MBH - M∗relation. WeutilizeNIR imagingfromtheHSTGOODS NICMOS Survey(a180orbitHSTprogramtoimagetheGOODS fieldintheH band)andthePOWIR SurveyandcombinethistothedeepestavailableChandraX-raydata. Byconstructingavolumelimitedsampleof120activegalaxiesat z < 3, weconstrainthepossibleevolutionin MBH – M∗ tobelessthanafactorof2. Moreover, weuseEddingtonargumentstocalculatethetotalfractionofmassivegalaxiesthatwillundergoanactivephaseintheirevolutionsincez=3, findingthatgreaterthan25%ofallmassivegalaxieswillachieveX-rayluminositiesintheSeyfertregimeorbrighter. FromthiswededucethatthethetotalenergyreleasedbyAGNsincez=3isgreaterthan15timesthetotalbindingenergyofallmassivegalaxiesintheUniverse, withinthisredshiftrange. Thiscolossalreleaseofenergymusthaveprofoundimplications
82 P30–P31
ontheevolutionofgalaxies, withmanyramificationstilltobeproperlyunderstood.
Theimpactoffeedbackontheorbitalcontentofdarkmatterhaloes.
SarahBryan (UniversityofManchester)withScottT. Kay, and Shude Mao
Galaxiesarethoughttoformhierarchically,throughthemergingandaccretionofsmallersystems. Assuch, thereshouldbeobservationalsignaturesofthesemergingprocessesintheremnantgalaxy, providingdynamicalinformationaboutitsformationhistory. Weinvestigatetheorbitalcontentofdarkmatterhaloesinordertoexplorewhatobservationalsignaturesmayresult.Todothis, wehaveusedtheOverWhelminglyLargeSimulations, asetofstate-of-the-arthighresolutioncosmologicalhydrodynamicalsimulationsrunwithdifferentphysicalprescriptionsforthefeedbackprocesses. Wequantifytheeffectsofthefeedbackprescriptionsonthedynamicsandorbitsofthedarkmatterandstellarparticles, bycomparingrunswithnofeedback, withstellarfeedbackandwithfeedbackfromAGN.Wecompareresultsofspectralanalysisoftheorbitalcontentofthesesimulationsandquantifythechangeinfractionofboxorbitsasdifferentimplementationsoffeedbackareconsidered, illustratingtheinfluenceoffeedbackprocessesontheorbitalcontentofthehaloes. Wealsoinvestigatehowtheorbitalcontentofthesehaloesdependonseveralkeyparameterssuchastheirmass, redshiftanddynamicalstate.
Theorientationofaccretiondisksandjetsinquasars
EmilyDown (UK GeminiSupportGroup)withSteve Rawlings, Devinder Sivia, and Jo Baker
I willdescribehowtheorientationofasampleof19high-zquasarswasmeasuredby(i)fittingthebroadH-αlinewithamodelwhichincludestheemissionfromaflattened, extendedaccretiondisk; and(ii)bymodellingtheradiospectralenergydistributionwiththeassumptionthatthejetsareDoppler-boosted. Resultsare: (i)Theopeningangleoftheobscuringtorusisconsistentwithpredictionsoftherecedingtorusmodel; (ii)Apossiblez-dependentvelocityoffsetbetweenthenarrowlineregionandtheaccretiondiskisfound;(iii)Misalignedaccretiondisksandradiojets, apossiblesignatureofarecentgalaxymerger, arerare.
TheEnviromentsofAGN atz1JamesFalder (UniversityofHertfordshire)with
Jason Stevens, and Matt Jarvis
WepresentananalysisofalargesampleofAGNenvironmentsatz∼ 1 usingstackedSpitzerdataat3.6um. Thesamplecontainstype-1andtype-2AGN intheformofquasarsandradiogalaxies,andspansalargerangeinbothopticalandradioluminosity. Wefind, onaverage, that2to3massivegalaxiescontainingasubstantialevolvedstellarpopulationliewithina200-300kpcradiusoftheAGN,constituting a > 8σexcessrelativetothefield. Secondly, wefindevidencefortheenvironmentalsourcedensitytoincreasewiththeradioluminosityofAGN,butnotwithblack-holemass. ThisisshownfirstbydividingtheAGN intotheirclassicalAGN types, whereweseemoresignificantover-densitiesinthefieldsoftheradio-loudAGN.IfinsteadwedispensewiththeclassicalAGN definitions, wefindthatthesourceover-densityasafunctionofradioluminosityforallourAGN exhibitsapositivecorrelation. One
interpretationofthisresultisthattheMpc-scaleenvironmentisinsomewayinfluencingtheradioemissionthatweobservefromAGN.Thiscouldbeexplainedbytheconfinementofradiojetsindenseenvironmentsleadingtoenhancedradioemissionor, alternatively, maybelinkedtomorerapidblack-holespinbroughtonbygalaxymergers.
TheroleoffeedbackinMilkyWaysatellitegalaxyformationusinghighresolutionsimulations
SamGeen (OxfordAstrophysics)withAdrianne Slyz, and Julien Devriendt
Weusesub-parsecresolutionhydrodynamicsimulationsoftheMilkyWayathighredshifttoinvestigatetheformationoftheMilkyWaysatellitegalaxies. Weanalysetheinfluenceofsupernovafeedbackondwarfgalaxyformation, andtheefficiencyofreionisationinsuppressingstarformationinthesmallestgalaxies. Bylocatinggalaxiesinourhighredshiftsimulationandtrackingthemtoz=0usingahalomergertree, wecancompareourresultstopresent-dayobservationsandcommentonthehypothesisthatreionisationhaltsstarformationinthelowestmasshalos. Wealsoconsidertheeffectofaddinggasphysicstosimulationsoftheformationofdwarfdarkmatterhalos, andtheimpactthishasonthemissingsatelliteproblem.
ClusterandGalaxyEnvironmentsofQuasarsKathrynHarris (JeremiahHorrocksInstitute,
UCLan)with R.G. Clowes, I.K. Sochting,G.M. Williger, L. Haberzettl, L.E. Campusano, and
M.J. Graham
Usinggalaxyclustersandquasarsitispossibletolookatthelargescaleenvironmentofquasarsandthereforeinferwhichformationmechanisms(e.g.,mergers, hotgastheory, galaxyharassment)aremostlikelytooccur. Lookingatthisoverarangeofredshiftsandquasarluminositiesgivesanindicationofanyevolutionofthisrelationship.
UsingCanada-France-HawaiiTelescope(CFHT),CosmicEvolutionSurvey(COSMOS) andImamoriMagellanArealCameraandSpectrograph(IMACS)data, galaxyclusterredshifts, positions, andshapesweredetermined. Wherepossible, directionalinformationwasconservedinordertogivemoreenvironmentalinformation. Thisdatacoversanareaof4sq. degreesintotalandextendstoaredshiftof0.8fortheIMACS dataand1.3fortheCOSMOS data.
Preliminaryresultsshowthequasarsappeartoliepreferentiallyinadirectionperpendiculartothemajoraxisoftheclusterassociatedwithit. Thisdoesnotchangeovertheredshiftrange0.2-0.8.Preliminaryresultsalsosuggestthatathigherredshifts(z < 0.5)quasarsliefurtherawayfromtheclustersthanatlowerredshifts, withquasarsatredshiftslessthan0.25lyingonaveragebetweentwoandfourMpcfromtheclusterandforz > 0.5 theaverageisthreetosixMpc.Thesedistancesareproject2D distanceandtakenattheredshiftofthequasar.
DiskHeating: ComparingtheMilkyWaywithCosmologicalSimulations
ElisaHouse (JeremiahHorrocksInstitute, UCLan)with C.B. Brook, B.K. Gibson, P. Sanchez-
Blazquez, and S. Courty
Wepresenttheanalysisoffivesimulationsrunwithdifferentparticleandgrid-basedcosmologicalhydrodynamicalcodesandcomparethemwith
observationaldataoftheMilkyWay. Westudythevelocitydispersionversusagefordiskstarsatz=0andfindthatthreeofthesimulationsaremoreconsistentwithobservationsbyHolmbergetal.(2008)wherethestellardiskappearstoundergocontinual/secularheating. TheothertwosimulationsareinbetteragreementwiththeQuillen&Garnett(2001)observationsthatsuggesta``saturation"intheheatingprofileforyoungstarsinthedisk. Wealsoanalysethekinematicsofdiskstarsatthetimeoftheirbirthfordifferentepochsinthegalaxy'sevolutionandfindthatinsomesimulationsstarsareborncoldwithinthediskandheatduetoacombinationofphysicaland/ornumericalprocesses, whileothersimulationspossessstellarpopulationswhichpresentlittleornoheatingwithtime. TwoofthemodelswhichareinbetteragreementwithobservationsoftheMilkyWay'sstellardiskundergosignificantlylowerminor-merger/assemblyactivityafterthelastmajormerger, i.e. oncethediskhasformed. Allofthesimulationsaresignificantly'hotter'thantheMilkyWaydisk, aproblemlikelyrootedintheunderlyingtreatmentoftheheatingandcoolingoftheinterstellarmedium, andtheresolution-dependentdensitythresholdforstarformation.
TheMulti-facetedX-rayactivityofthecomplete3CRR AGN sampleatz<0.1
ElizabethMannering (UniversityofBristol)withM. Birkinshaw, D.M. Worrall, D.A. Evans,M. Hardcastle, R.P. Kraft, and E.S. Perlman
WepresentChandraimagesof9previouslyX-rayunobservedsourcestocompleteobservationsofthe3CRR low-redshiftradiogalaxysample. The36sourcesofthecompletesamplealsohaveexcellentmulti-wavelengthradiodataandhavebeenimagedwithSpitzer(3.5-160microns)andwithHST.ThesamplespanstheimportanttransitioninradioluminositiesandmorphologyfromFRI toFRII type. Theimagingandspectroscopyofthecores, jets, hotspotsandatmosphereswillbeofpermanentlegacyvalue.Thispostergivesafirstlookatthesedataandindicateshowweplantoinvestigateparticleaccelerationmechanisms, interactionsbetweenradioplasmaandtheISM andIGM,theemissionmechanismofhotspots, andAGN fuelling
MomentumdrivenfeedbackfromstellarnucleiRachaelMcQuillin (KeeleUniversity)
InthelastdecadeobservationswiththeHubbleSpaceTelescope(HST) haverevealedthepresenceofmassivestarclustersatthecentresofthemajorityoflowandintermediatemassgalaxies.Anunexpectedobservationalresultisthatnuclearclustermass, Mnc, scaleswiththevelocitydispersionofthehostgalaxybulge, σ. TheMnc − σ relationisanalogoustothatbetweenthemassesofcentralsupermassiveblackholes(SMBHs)andthevelocitydispersionsoftheirhostgalaxybulges. Theobserved M–σ relationcanbeunderstoodasaconsequenceofmomentumconservingfeedbackfromthenucleuswhichsweepstheambientmediumintoashellthatexpandsintothegalaxy. Thereisacriticalmassofthenucleusforwhichtheshellcanescapethegalaxyhencecuttingoffthegrowthofthenucleusandlockinginthe M–σ dependence. Previousworkhasmodelledthisprocessingalaxieswithsingularisothermaldark-matterhaloes. Inthiscontribution, weextendthisworkandinvestigatethe M–σ relationthatresultsfromnuclearfeedbackingalaxieswithmorerealisticdark-matterandgasdensityprofiles.
P31 83
TheColdGasContentofBulgelessDiskGalaxiesKatePilkington (JeremiahHorrocksInstitute,UCLan)with Brad Gibson, ChrisB. Brook,
Greg Stinson, and Francesco Calura
Wepresentananalysisoftheneutralhydrogen(HI) propertiesofasetoffullycosmologicalhydrodynamicaldwarfgalaxysimulations. AsreportedrecentlybyGovernatoetal. (2010), thesesimulationsarethefirstoftheirkindtoresultinthesuccessfulreproductionofa(dwarf)spiralgalaxy,withoutanyassociatedstellarbulge. Inablindexperiment, wehavenowsetouttocompareindetailtheHI distributionandkinematicsofthesesimulatedbulgelessdiskswiththoseofthreecomparabledwarfsfromtheTHINGS (TheHINearbyGalaxySurvey)archive. Wewishtoanswerthequestion"Arethegaspropertiesofthefirstsuccessfullysimulatedbulgelessdwarfsconsistentwithobservations?". Todoso, wehavethusfarextractedfromthesimulations, radialandverticaldensityprofiles, scalelengths, andspatially-resolvedmapsofscaleheights(eg.flaring, warping)andvelocitydispersion(eg.velocityellipsoid, turbulence). Ourhighestresolutiondwarfshowsseveraluniqueandchallengingcharacteristics(relativetotheTHINGSobservationsofcomparabledwarfs)whichweareinthemidstofquantifying, including(i)ahigh-densitycoldgascorewithintheinner1kpc(10timesthedensityatoneHI diskscalelength), (ii)significant, andcontinual, diskflaringfromtheinnertotheouterHI disk(factorof10increaseinscaleheightperdexincreaseinradius), and(iii)asignificantly(kinematically)colderHI disk(factorof5lowerlines-of-sightvelocitydispersions,relativetoHoII,NGC4214, andIC2574). Wewilldiscusstheramificationsofourpreliminaryanalysesintermsofthedefiningrolesplayedbyenergyfeedbackandstarformationthresholdsinsuchcosmologicalhydrodynamicalsimulations.
SearchingforComptonThickAGN atz2indeepX-rayfields
CyprianRangel (ImperialCollegeLondon)withKirpal Nandra, Elise Laird, and James Aird
CurrentlytheX-rayemissionfromAGN failstofullyaccountfortheobservedX-rayBackground(XRB) atharderenergies. IthasbeentheorizedthisisduetoapopulationofobscuredAGN thatwehaveyettoobserve. ComptonThick(CT) AGNhaveobscuringgasofthesurroundingtoruswithNH > 1024 cm−2, thustheX-rayemissionfromthecentralsourceisheavilysuppressed. WepresenttheresultsofasearchforCT AGN atz∼ 2
indeepX-rayfields. WeidentifyX-raydetectedAGN throughLikelihoodRatio(LR) matchingofopticalandNIR photometrytoX-raydata.SometimesCT AGN aredetectedviascatteredorreflectedX-rayemissionfromthecentralsource,butatz∼ 2 suchtheseprocessesmaybetoofainttoyieldadetection. StackingisthereforeusedtotestforthepresenceofX-rayemissionfromcandidateCT sourcesselectedviatheirmulti-wavelengthproperties.
StellarFeedbackinSPH GalaxyFormationSimulations
GregStinson (JeremiahHorrocksInstitute, UCLan)with Chris Brook(UCLan), Jeremy Bailin(Michigan), Sarah Nicerkson(McMaster),
Hugh Couchman(McMaster), and James Wadsley(McMaster)
WepresentastudyofgalaxiesandtheiraccompanyingsatellitedwarfgalaxiesfoundintheMcMasterUnbiasedGalaxySimulations, aseries
of15cosmologicalSPH simulationsofMWmassedobjects. Inthesesimulationsthatformarangeofgalaxymorphologies, wefindthatthesatelliteluminosityfunctionsaresimilartowhatisfoundintheLocalGroupwheneffectivestellarfeedbackisutilized. Oneoftheproblemswiththegalaxiesformedinthesesimulationsisthedensecentralconcentrationofmatterfoundineverygalaxy. Weexplorepossiblesolutionstothisproblemusingalternatestarformationandstellarfeedbackrecipes.
Superstarclusterfeedbackfromlocaltogalaxyscales
MarkWestmoquette (UCL)
Understandingstarburst-drivenoutflowsisimportantformanyreasonswithinthecontextofgalaxyevolution. However, tounderstandoutflowsonthelargescale, thedetailsoffeedbackmechanismsfromindividualstarclustersmustfirstbeunderstood. I willdiscussrecentresultsfromanumberofhighspatialandspectralresolutionintegralfieldspectroscopicstudiesoftheionizedgasenvironmentwithinasampleofnearbystarbursts. Thesestudiesareallowingustobuildupapictureof(1)howpowerisfedfromsuperstarclustersintothesurroundingISM,(2)howtheISM propertiesaffecthowthispowerisdirected,and(3)howthegasoutflowsevolvestructurallyandenergeticallytowardsthelarger-scales.
StabilityandevolutionofclustergalaxiesinMOND
XufenWu (PhysicsandAstronomy, UniversityofStAndrews)with Hongsheng Zhao, Yougang Wang,
Benoit Famaey, and Martin Feix
FollowingSchwarzschild'sapproach, weconstructaseriesofHernquistmodelsembeddedinexternalfieldsintheframeworkofMOdifiedNewtonianDynamics(MOND).Thesemodelsrepresentmedium-massellipticalgalaxieswithmildcuspswithinagalaxycluster, providingaMONDianexternalfieldontheorderof gext ≈ a0. UsingN-bodysimulations, wefurthertestthestabilityofthesemodels. WefindthattheSchwarzschildmodelsarenotinrigorousequilibrium. Theoutskirtsofthegalaxiesdeveloplopsidedshapesalongtheexternalfield'sdirection, andtheradiicontaining 90%ofthetotalmassincreasebyafactorof 2 during 60 simulationtimes(NewtonianKepleriantimesatscalelengthof 1kpc)afterwhichthemodelsseemtosettletoastableequilibrium. Comparingourresultstoanisolatedgalaxymodel, theSchwarzschildmodelsinexternalfieldsarelessself-consistentandstable.
P32StellarmagnetismthroughtheeyesoftheFORS1
instrumentoftheESO VLTStefanoBagnulo (ArmaghObservatory)with
L. Fossati, C. Izzo, J.D. Landstreet, C. Folsom, andO. Kochukhov
Duringafulldecadeofoperations, theFORS1instrumentoftheESO VeryLargeTelescopehascollectedalargeamountofmagneticfieldmeasurementsofvariouskindsofstars. TogetherwiththeESPaDOnS instrumentoftheCanada-France-HawaiiTelescope, withtheMuSiCoS andNARVAL instrumentsofthe2mTelescopeBernardLyotofthePic-du-MidiObservatory,FORS1hasbeenoneoftheworkhorseinstruments
fortheobservationalstudiesofstellarmagnetism.Severalinterestingdetectionswereobtained, someofthemwereeventuallyconfirmedbyfollow-upinvestigations, somewerenot. Wehaveperformedahomogeneus(re-)analysisofthefullFORS dataarchive, andinthistalkwewillgiveanupdatedreviewoftheincidenceofthestellarmagnetisminvariousclassesofstars.
InvestigatingtheX-rayEmissionofA-typeStarsThroughtheMagneticActivityofUnresolved
LowerMassCompanionsRobertDeRosa (UniversityofExeter)with
J. Bulger, J. Patience, B. Leland, and B. Macintosh
WepresenttheresultsofaninvestigationintothesourceofX-rayemissionfromnearbyearly-typestars. ByutilisingtheROSAT All-SkySurvey(RASS) brightandfaintsourcecatalogues, andthepreliminaryresultsfromourongoingmultiplicitysurveyofA-typestars.
Bremsstahlungemissionhasbeendetectedfromnumerousmain-sequencestars, fromO-M.StudiesofmassivestarsshowX-rayluminosityscalingasafunctionofthestellar-winddensity, suggestingthatthesestrongradiativelydrivenwindsaretheprimarygeneratingmechanism. ForlessmassivestarstheX-raygenerationisthoughttobeduetoadynamoeffectcausedbydifferentialrotation. Starsfrommid-B tolate-A haveinsufficientluminositytodrivemassivewinds, norhavesufficientlydeepconvectiveenvelopesandshouldtheoreticallyhavelowX-rayemission. Contrarytothesepredictions, X-rayemissionhasbeendetectedfromnumerousnearbyA-typestars. Thedetectionoftwolow-massstellarcompanionstoX-rayemittingA-typestars(e.g. AlcorB) wouldsuggestanX-raygenerationmechanismfortheseanomalousstars- unresolvedcompanions.
WithinthisstudywehavecompiledadistancelimitedsampleofnearbyX-raydetectedA-typestars, alongsideacontrolsampleofnonX-raydetectedA-typestars. Thetypicalangularresolutionachievedinourobservationswas∼ 0.1"withthenarrowbandexposuresallowingustoresolve ∼ 10AU binaries, whilstsensitivitytothebottomofthemainsequencewasachievedat∼ 1 − 2"withthelongerbroadbandexposures.WefindthatagreaterproportionofX-raydetectedA-typestarshaveanassociatedcompanioncomparedwiththoseinthecontrolsample,suggestingthatunresolvedlow-masscompanionsareindeedasourceofA-starX-rayemission.
TestingtheabilityoffieldextrapolationmodelstopredicttheX-raypropertiesofpre-mainsequence
starsScottGregory (UniversityofExeter)with
E. Flaccomio, C. Argiroffi, J. Bouvier, J.-F. Donati,E.D. Feigelson, K.V. Getman, G.A.J. Hussain,M. Ibrahimov, M. Jardine, and F.M. Walter
Byextrapolatingfromobservationallyderivedmagneticsurfacemaps, obtainedthroughZeeman-Dopplerimaging, modelsofstellarmagnetospherescanbeconstructed. Byassumingthattheplasmatrappedalongtheclosedfieldlinesisinhydrostaticequilibrium, coronalX-rayemissionproperties, suchastheglobalX-rayemissionmeasureandtheamountofrotationalmodulationofX-rayemission, canbepredicted.Forpre-mainsequencemagnetospherestheanalysiscanbeextendedtoincorporateaccretionflows, andpredicttheamountofsofterX-rayemissionfromaccretionspotsthatwouldbeobserved. I willdetailthepreliminaryresultsofanambitiousmulti-wavelength, multi-observingsite,
84 P31–P32
andnearcontemporaneouscampaign, combiningspectroscopicoptical, nIR,UV,X-ray(200ks,Chandra), spectropolarimetricandphotometricmonitoringoftheaccretingpre-mainsequencestarV2129Oph. Surprisinglythenewmagneticmapderivedfromthe2009dataappearstoindicatethatthesurfacemagneticfieldhasundergonelittleevolutionsinceitwaspreviouslyobservedin2005. ThedatasetalsoallowsX-rayemissionfromthestellarcoronaandtheaccretionhotspotstobedisentangledandcruciallyallowsthevalidity, andthepredictions, ofthe3D fieldtopologiesderivedviafieldextrapolationtobecriticallyexamined.
Stellarmagnetisminsolar-typestarsGaiteeHussain (ESO)
Magneticfieldsplayaroleatalmostallevolutionarystagesoflowmass(F toM-type)stars.Onthepre-mainsequence, strongkG fieldschannelaccretionfromcircumstellardisksontothecentralT Tauristars; whileinolderplanet-hostingsystemswefindevidenceofmagnetosphericinteractionbetweenplanetsandtheirhoststars.
ZeemanDopplerimagingtechniquesenableustomapstellarsurfacemagneticfieldsinunprecedenteddetail. Magneticfieldmeasurementsmadefrommagnetically-sensitiveintensitylineprofilesfurthercomplementandenhancetheinformationgainedfromthesesurfacemagneticfieldmaps. Thelatestresultssuggestthatthesizeandcomplexityofsurfacemagneticfieldsdifferinfullyconvectivestarsandstarswithradiativecores. A furthertransitionoccursasstarsspindownovertime.
I willreviewourcurrentunderstandinganddemonstratehowmagnetosphericmodelsoflowmassstarsbasedonsurfacemagneticfieldmapsaretestedusingmulti-wavelengthobservations.Finally, I willgiveanoverviewoftherichfutureprospectsofthisfieldinlightofnewinstrumentsandfacilities, bothintheshortandlong-term.
MagneticactivityinfastrotatingM-dwarfsaboveandbelowthefullyconvectiveboundary
RobJeffries (KeeleUniversity)with Richard Jackson
WepresentresultsfromsurveysofcoronalandchromosphericactivityamongfastrotatingM-dwarfsbelongingtotheyoungopenclustersNGC2547andNGC 2516. OurtargetsarecoolclustermemberswithknownrotationperiodscoveringspectraltypesfromK3toM5. Coronalactivityappearstobecontinuousacrossthefullyconvectiveboundary, wherealmostallthefullyconvectivestarsexhibitsaturatedX-rayemission.However, thelevelofsaturatedchromosphericemissiondeclinesbyfactorsof2-3forstarsofspectraltypeM3andcooler, coincidingwithboththefullyconvectiveboundaryandadramaticincreaseinaveragerotationrates. Noevidencefor"supersaturation"wasfoundinthechromospheresorcoronaeoftheM-dwarfs. Wediscussthesefindingsintermsofchangingmagnetictopologies.
TheDopplerShadowofWASP-3bGrantMiller (UniversityofStAndrews)
Hot-jupiterplanetsforatlargedistancesfromtheirhoststarsthenmigrateinwardstotheirobservedorbitalseparations. Themechanismsresponsibleforthisarenotfullyunderstoodbutthespin-orbitalignmentofthesystemgivescluesastohowtheplanetsmigrated. Thespin-orbitalignmentcanbemeasuredbyanalysingtheRossiter-McLaughlin
effect. Thisistheradialvelocityanomalycausedbyaplanetasittransitsthestellardisc. WedescribeanewtomographicmethodforanalysingtheRossiter-McLaughlineffectandpresenttheresultsofitsapplicationtotheWASP-3system.Wealsoexplainhowthismethodcanbeusedtoconfirmtheexistenceofplanetsaroundearly-typestarspreviouslyinaccessibletoplanethuntersduetotheirrapidrotationandlackofspectrallines.
Theinfluenceofthestellarwindonclose-ingiantplanets
AlineVidotto (UniversityofStAndrews)withM. Opher, V. Jatenco-Pereira, and T.I. Gombosi
Sincethefirstdiscoveryofextrasolarplanets, morethan300planetshavebeendetected, manyofthemlocatedverynearthehoststar. Becauseofsuchextremeproximity, interactionoftheplanetwiththestarisexpectedtogiverisetoavarietyofphenomena. Thestellarwindisexpectedtodirectlyinfluencetheplanetanditsatmosphere,e.g., bychangingtheconfigurationoftheplanet'smagnetosphere, producingnonthermalplanetarymagnetosphericradioemissions, etc. Sofar, thefewtheoreticalworksinvestigatingtheinfluenceofthestellarwindonthemagnetosphereofplanetswerebasedonsimplifiedtreatmentsofthestellarwinds. Wedevelopedthree-dimensionalmagnetohydrodynamicsmodelsofstellarwindswhichenabledustodetermineself-consistentlythecharacteristicsoftheimpactingwindontheplanet. Underrealisticstellarwindconditions, weanalyzedtheinfluenceofthewindonplanetmigrationbyestimatingthemigrationtime-scaleduetodragforcesexertedbythestellarwindonahot-Jupiter. Furthermore, wealsoestimatedthepowerreleasedfromthemagneticinteraction(reconnection)betweenamagnetizedwindandthemagnetosphereofaclose-ingiantplanet. Weshowthatthecharacterizationofthewindpropertiesofthehoststarisessentialforadeeperunderstandingofextrasolarplanetarysystems.
P33Astronomyinthecurriculum. Developmentsat
KS4andKS5CharlesBarclay (MarlboroughCollegeandOxford
Astrophysics)
Educationisthefuture. Childreninfluenceparents('thepublic')andthencepoliticalperceptionofasubject'simportance. IfinherententhusiasmforAstronomyatages10and11canbemaintainedwiththepotentialofaqualificationatGCSE,IbelievepupilenthusiasmforSciencecanbeenhancedwiththeaddedbenefitthatthesubjectisequallyappealingtobothgirlsandboysatthislevel. TheGCSE inAstronomycontinuestogrowexponentiallyandthenewSpecification,developedwithschoolteachersandprofessionalastronomers, implementedin2009forfirstexamin2011, lookstoseeanotherhikeinpupilnumbers. AtKS5, thedevelopmentoftheExtendedProjectinitiativealsoallowsforin-depthpupilmotivatedstudyofastronomicaltopicsinthesixthform. I willoutlinethecurrentpositionanddiscussthepotentialofthesequalifications
TheBigBang!DanielleBewsher (JeremiahHorrocksInstitute,
UCLan)with D.S. Brown, J.M. Wild, L.M. Green,G.M.H. Wilkins, M. Marsh, C. Alexander, J. Kelly,S. Dalla, R.W. Walsh, H.E. Mason, and M. Popescu
The'BigBang'isanationalSTEM outreachactivitywhichstartedNationalScienceweekin2010. TheUniversityofCentralLancashireledacollaborationofsolarphysicistsfromaroundtheUK toproducethe'LivingwithaStar'exhibitionstandattheBigBang. Thispresentationwilldiscussthehighs/lowsandpitfallsoforganisingsuchevents!
OutreachduringInternationalHeliophysicalYearLucieGreen (UniversityCollegeLondon–MSSL)
2007to2009wasdesignatedasInternationalHeliophysicalYeartocelebrate50yearsofspacescienceandsolarsystemphysics. TheUK joinedinwithaseriesofeventswhichranacrossthecountry. Thistalkwillgiveanoverviewoftheactivitiesthattookplaceandlessonslearned.
DevelopmentofanAll-SkyCameraforOutreachActivities
MartinHendry (UniversityofGlasgow)withGiles Hammond
TheChargeCoupledDevices(CCD's)foundincommercialCCTV camerasofferhighsensitivityatlowcost. However, intheiroff-the-shelfformthesecamerasarelimitedtoamaximumexposureof1/5sbyanelectronicshutterandarethereforeoflittleuseforimagingdeepskyobjects. WithminormodificationstothecircuitboarditispossibletodisablethisshutterandcontroltheclockpulseswhichareusedtoreadouttheCCD.Thisallowsforlow-lightimagingofastronomicalobjects.
Overthepastcoupleofyearsanall-skycamerahasbeendevelopedattheAcreRoadObservatory,UniversityofGlasgow. ThisdevicecomprisesaCCTV surveillancecamerainaweatherproofboxwithanacrylicdome. A wideangle(1.6mmfocallength)lensisattachedtothefrontofthecameraandthisoffersanalmostfull180degreefieldofview. Byadjustingtheexposurelengththecameraisabletooperatebothindaylightandalsoduringthenight. Fromtheurbanlocationoftheobservatorythisallowsobservationofbrightstarsandthemoon/planetstogetherwithobservationofcloudstructuresandotherinterestingmeteorologicaleffects.
Thecaptureprogram(developedinMATLAB) iscapableofrunningonanyWindowsXP machine(connectedtotheinternet)andautomaticallyselectsthecorrectexposure/savestheresultingimageasaJPEG.Theseimagescanthenbecombinedintoamoviefortheday. A secondcameraisnearingcompletionanditwouldbeidealifaschool/astronomicalsocietywithadarkskylocationwouldbewillingtohostthisdevice.Theimagesfromthecameracouldbeuploadedtotheinternetandwouldbeanexcellentoutreachandlearningtool.
TheScottishSolarSystemMartinHendry (UniversityofGlasgow)
AspartofaScotland-wideprogrammeofpublicoutreachforIYA2009, the"ScottishSolarSystem"projectwasapartnershipbetweenGlasgowUniversity, GlasgowScienceCentreand14Scottishastronomyclubsandsocieties. Theprojectcoordinatedarangepubliceventsacross
P32–P33 85
thecountry, heldatlocationswhich- withGlasgowScienceCentreastheSun- duringAutumnMoonwatchweekcreatedascalemodeloftheSolarSystem, withcorrectlyscaledphysicalobjectsateachoftheplanetarylocations.
InthistalkI willbrieflyreviewthesuccessesoftheScottishSolarSystemproject, andconsideritslegacyforfutureastronomyoutreacheventsinScotlandandbeyond.
IYA 2009ontheBigIslandofHawaiiIngeHeyer (JointAstronomyCentre)with
Janice Harvey(GeminiObservatory),Peter Michaud(GeminiObservatory),KumikoS. Usuda(SubaruTelescope),
Gary Fujihara(UniversityofHawaiiatHiloInstituteforAstronomy), and Shawn Laatsch
(`ImiloaAstronomyCenterofHawaii)
TheInternationalYearofAstronomy(IYA) 2009combinedtheoutreacheffortsofalltheobservatoriesonMaunaKea, whichincludestheUnitedKingdomInfraredTelescope, theJamesClerkMaxwellTelescopeandtheGeminiNorthObservatory. IYA allowedtheMaunaKeaObservatoriesOutreachCommittee(MKOOC) tobrandourannuallocaleventswhiledevelopingseveraluniqueandinnovativeactivitiesandproducts. OurflagshipJourneythroughtheUniverse(JTTU) programmeintroducedtheGalileoscope. JTTU’steachertrainingprogrammesandfamilyscienceeventswereenhancedwithIYA cornerstoneactivities. Bycollaboratingwithourlocalnewspaper, 70,000copieswerepublishedofaspecialtabloid“StarsOverMaunaKea”. OurgroupadditionallycontractedawebsiteonIYA onthelocalnewspaper’swebsitewhichin2009receivedover1.7millionhits, andwhichhasbeencontinuedforthisyear. AstronomytradingcardswereproducedforourlocalAstroDayandtheGalileoBlockParty, thelatterbeingoureventfortheGalileanNightsinvitingtheentirelocalcommunitytotheobservatoryfacilities. A postercontestencouragedlocalstudentstocombineastronomyandtheirculturalbackgroundinauniqueartisticexpression. A year-longfreecollege-levelintroductoryastronomyclassgavelocalteachersastronomycontentandteachingtoolsfortheirclassroomsatallgradelevels. Thedirectorsofallobservatoriesgavemonthlypublicpresentationsintwolocationsonourisland, andtheMaunaKeaObservatoriesleadoffthe80-Telescopes24-hourwebcast. Photosandactivitiesfromalleventshavebeenarchivedonourwebsitestosharewiththeworld.
UK DarkSkyDiscoveryDanHillier (RoyalObservatoryEdinburghVisitor
Centre)
TheDarkSkyScotlandprogrammehasbeenrunningforthreeyearsinvolvingresearchastronomers, astronomystudents, amateurastronomersandsciencecommunicatorsinmorethan60publiceventsatlocationsthroughoutScotland. IthasestablishedDarkSkyDiscoverySitesinlocalcommunitiesandaStargazersWelcomeschemefortourismbusinesses. UK DarkSkyDiscovery, 2010-2012, aimstorunsimilarprogrammesthroughouttheUK basedonsimilarpartnershipsinWales, NorthernIrelandandtheEnglishregions.
Beyondconstellationstories: communicatingcutting-edgescienceandengagingnewaudiencesthroughnovelplanetariumprogrammingforthe
InternationalYearofAstronomyOliviaJohnson (RoyalObservatoryGreenwich)
with Claire Bretherton(CarterObservatory), andMarek Kukula(ROG)
Ofthe1.4millionvisitorsattractedbythewiderangeofexhibits, events, talks, andworkshopsattheRoyalObservatoryGreenwich(ROG) duringtheInternationalYearofAstronomy(IYA),over130,000attendedaplanetariumshowatthePeterHarrisonPlanetarium(PHP).OpenedinMay2007, thePHP isnowtheonlyplanetariuminLondonandusestheprogrammableDigistar3systemtodeliveracombinationofliveandpre-recordedshowstoschoolandpublicaudiences.
DuringIYA,theScienceEducationteamattheROG explorednewwaysofexploitingtheintrinsicexcitementandsenseofconnectionwiththenightskyofferedbyimmersiveplanetariumshowstosupportandenhancethebroadrangeofsciencecommunicationeffortsacrosstheObservatory.Wewereparticularlyinterestedinmovingbeyondconstellation-basedtoursofthenightskytocommunicateup-to-the-minuteastronomicaldiscoveriesandengagenon-traditionalaudienceswithinthedome.
Inthistalk, I'llreportonavarietyofnewplanetariumcontentproducedattheROG duringIYA,including"VisionsofSaturn", developedincollaborationwiththeCassini-Huygensteamtoconveytheexcitementoftheirongoingresearchtofamilyaudiences, and"Sci-FiUniverse",developedincollaborationwiththeSci-FiLondonFilmFestivaltoengagefilm-goingaudiencesinthesciencebehindsciencefiction. Lookingtothefuture, I'llaskhowinnovativecollaborationwithplanetariacouldbenefitsciencecommunicationintheUK beyondIYA.
SongsoftheStars: theRealMusicoftheSpheresDonaldKurtz (JeremiahHorrocksInstitute, UCLan)
with R. Jain, M. Thompson, M. Roth, R. New,Y. Elsworth, W. Chaplin, I. Roxburgh, and
D. Gough
TheRoyalSocietySummerScienceExhibitionin2010willbeheldintheSouthbankCentreinLondonfor9daysfrom26Juneto4JulyincelebrationoftheRoyalSociety’s350thanniversary. Wewillhaveanexhibit, “SongsoftheStars: theRealMusicoftheSpheres”, thatwillbeabouthelioseismologyandasteroseismology.Aspartofouroutreachplanswehavemadetwoposters-- onegeneralforhomedisplay, andtheothermoredetailedforclassroomuse- thatwewillgiveawayas“freebies”tothousandsofthe30,000peopleexpectedtoattendtheexhibition.Our“poster”hereatNAM isthedisplayofthesetwofreebieposters, withsomecopiesavailableforyoutotakeaway, shouldyouwishtodoso. TheproductionofthepostershasbeensupportedbytheHelio- andAsteroseismologyNetwork(HELAS),aCoordinatedActionfundedbytheFP6-Infrastructure-ProgrammeoftheEuropeanCommission.
4YearsofPodcastingStuartLowe (TheJodcast)with JodcastTeam
Since2006wehavebeenproducingaregularpodcastcoveringastronomyandspacescience.Wereportasummaryofourexperiencesoverthepastfouryearsincludingourlistener/viewing
figures, feedbackandadescriptionofourliveepisoderecordedinlate2009.
SchoolsoutreachfortheGlasgowNAMAlecMacKinnon (UniversityofGlasgow)
PriortoNAM,pupilsinseveralschoolsaroundthegreaterGlasgowareahavebeenworkingonalittleresearchproject, findingoutalltheycanaboutsunspotsandforminganopinionontheroleofsolaractivityinclimatechange. Theywillpresentposterssummarisingtheirfindingsatasessiontoday. Wedescribehowandwhythisprojectwassetupandgiveatrailerforthepostersession.
Sun|trek- thefinalfrontierHelenMason (UniversityofCambridge)with
Sun|trekteam
Sun|trek(www.suntrek.org)isawebsiteabouttheSunanditseffectontheEarth. Itisaimedatschoolchildren. Itisgrowingfromstrengthtostrength, withover14,000userspermonthworldwide. Itisnowlinkedtomanywebsites(NASA,RAS,IoP,schoolscienceandtheBBC).WehavesomefundsfromSTFC toupdateSun|trekandwouldlikesomehelpandideasfromouryoungersolarresearchers. Findoutmore...
TheMusicoftheSunasaStarRichardMorton (UniversityofSheffield)with
R. Erdélyi
TheSun, atypicallate-typestar, isahighlydynamicplasmathreadedbyarathercomplexandubiquitousmagneticfield. Thismagneticfieldprovidesthefoundationsforawidevarietyofplasmastructureinthesolaratmosphere. Amongsuchstructuresaree.g. coronalloops(huge, oftenhundredsofMmlongmagneticloops), coronalholes(openmagneticstructures)orprominences(eruptivemagneticstructures, frequentlycausingdisruptionsinspaceweatherconditions). Becauseoftheirelasticnature, eachofthesemagneticfeaturesinthesolaratmospherecansupportanarrayofmagneto-hydrodynamic(MHD) oscillatorymodes. Fromaphysicalpointofview, therearetwofundamentallydistinguishabletypesofoscillatorymodesthatattractattention.Transversaloscillationsofcoronalloops, drivenexternallybyeruptivesolarflares, whichcanbethoughtofanalogoustosomeonepluckingaguitarstring. Ontheotherhand, therearelongitudinaloscillationsofmagneticloops, driveninternallybynano/micro-flares, whicharesimilartosomeoneblowingawindinstrument. Inthissense, theubiquitousmagneticoscillationsofthesolaratmospherearethemusicoftheSun!
Theoscillatorymodesofmagneticstructuresaredeterminedbytheinternalphysicalparametersofthesestructures(e.g., strengthofmagneticfield,temperature, density). ObservingtheMHDoscillationsprovidesauniqueandunprecedentedmethodforobtainingcrucialinformationabouttheotherwisedirectlyunobservable, internalpropertiesofsolaratmosphericplasma. Thistechnique, calledsolarmagneto-seismologyorcoronalseismology, isanalogoustothetraditionalseismologyoftheEarthwherefromdetectingearthquakesattheEarth'ssurface, geologistsderivetheinternalsub-crustpropertiesofEarth.
Magneto-seismologyisarapidlyemergingfieldofsolarandspacephysicsprovingunprecedentedinsightintosolarandstellarmagneticstructures.Themethodreliesonthecomparisonoftheoreticallyderivedpredictionstoobservations
86 P33
andapplyingtheobservationstodeterminetheotherwiseunmeasurable, localplasmaparameters,e.g. themuch-sought-aftermagneticfieldanditsfinestructureinthesolarcorona. Understandingaccuratelytheplasmapropertiesinthesolaratmosphereisvitalforthepredictionofspaceweatherevents, whichhaveadirectimpactonmannedspacemissions, lifehereonEarthandmaintainingpowergridsandsatellites.
BeyondIYA2009: SustainableScienceEngagement
SteveOwens (IYA2009)
FollowingthesuccessofIYA2009, agreatdealofmomentumandexpertiseinpublicengagementhasbeendevelopedamongsttheastronomycommunityintheUK.
Howmightthismomentumbesustained, andwhatisnextforUK astronomyoutreach?
SteveOwens, UK Co-ordinatorforIYA2009
TheSocietyforPopularAstronomy'sTelescopesforSchoolsProject
HelenWalker (STFC RutherfordAppletonLab)
TheSPA startedplanningfortheInternationalYearofAstronomy(IYA2009)inApril2007, anddecidedtheywouldtryandsend1000telescopesto1000secondaryschoolsintheUK.Theprojectprovedtobeagreatsuccessandaroundone-quarterofUK secondaryschoolsnowpossessa70mmrefractingtelescopewithsupportmaterials.Workingwithteachers, aDVD wasprofessionallyproducedwithinstructionsonhowtosetupandusethetelescope, alessonplan, interviewsandadditionalinformation. STFC fundedthepurchaseofthetelescopesandtheRAS fundedtheproductionoftheDVD.TheSPA providedanewareaontheirwebsitetosupportthethreemoonwatchperiodswhenschoolswereencouragedtousethetelescopes, andSPAvolunteerslookedaftertheproject. Over85%oftheschoolswhorespondedtoasurveyattheendoftheyearsaidthetelescopewasavaluableadditiontotheirschoolsresources. Aroundtwo-thirdsoftheschoolshaduseditmorethanfivetimes, andtherewereover200entriesinthecompetitionforMoon-relatedartwork. Itisestimatedthatmaybe25,000to50,000childrenhavelookedthroughoneofthetelescopesduringIYA2009.
ChallengesofPublicEngagementwithChildreninCare
AlisonWallace (UniversityCollegeLondon–MSSL)
Childreninpubliccareareyoungpeoplewhoareinthecareoflocalauthoritiesorwhoarelookedafterbyfostercarersorinchildren'shomes. Thesechildrenaremorelikelytofallbehindatschoolwithonly13%ofattainingfivegoodGCSEscomparedwith62%ofallchildren. Theyalsohaveamuchhigherstatisticalchanceofbecomingunemployedwhentheyleaveschool. Therearearound60,000childreninpubliccareintheUK atanyonetimeandweexaminethechallengesfacedbythespacesciencecommunitytoengagewiththem. Wediscussthereasonsthatchildrenincarearelesslikelytoachievetheirpotentialandthefactorsthatshouldbetakenintoaccountwhenorganisingactivitiesforthem. WeinvestigateongoingschemesincludingtheLetterboxclubandlookatthefuturedirectionofoutreachactivitiesincludinganoutlineofaproposedprojectatUCL-MSSL.
DidtheSunEarthPlanworkout?JimWild (LancasterUniversity)with
sunearthplan.netteam
sunearthplan.netisaSTFC-fundedpublic-facingoutreachprojectdesignedtoinformthegeneralpublicoftheimportanceofsolarsystemresearchandhighlighttheUK'sleadingroleinthisfield. Inordertoachievethisaim, theprojecthasbroughttogetherresearchscientists, professionalweb-designersandpublishedsciencewriters.LaunchedinFebruary2007, tocoincidewiththelaunchoftheInternationalHeliophysicalYear, thesitehasattractedover400,000uniquevisits(withmonthlyvisitspeakingatnearly20,000)andinterestfromboththeonlineandtraditionalmedia. Visitorfeedbackindicatesthatthemajorityofvisitorsarewithinthetargetaudience- adultmembersofthegeneralpublicunconnectedwithscienceorteaching, roughlyhalfofwhichwerepreviouslyunawareofUK activitiesinspaceresearch. Assuch, sunearthplan.netisasuccessfulandcost-effectiveexampleofanonlinescienceandtechnologyoutreachproject. Inthispresentationwehighlighttheproject'ssuccesses,reflectonthegreatestchallengesandsummarisethelessonslearnedthatmightbeappliedtootherprojectsinthefuture.
P34Magneticfluxemergenceandcoronaleruptions
intheSunVasilisArchontis (UniversityofStAndrews)with
AlanW Hood
Oneofthemostimportantprocesses, responsibleformanydynamicalphenomenaobservedintheSun, istheemergenceofmagneticfluxfromthesolarinteriorinactiveregionsandthemodificationofthecoronalmagneticfieldinresponsetotheemergence.
Inthistalk, wepresentnewresultsfrom3DnumericalMHD models, whichhavebeenusedtostudytheprocessofmagneticfluxemergenceintosuccessiveatmosphericlayers. WediscusstherecentprogressandtheconnectionbetweenfluxemergenceandpossibleinitiationmechanismsoferuptiveeventsintheSun.
Medium- andsmall-scaletransientsinthesolarwind
MarioBisi (AberystwythUniversity)withA.R. Breen, G.D. Dorrian, J.A. Davies, and
R.A. Fallows
Co-ordinatedobservationsofwhite-lightscatteringfromthesolarwindmadebytheSTEREOheliosphericimagers(HIs)andinterplanetaryscintillation(IPS) fromtheEISCAT facilityinMay2007revealedthepresenceofsignificantsmall-andmedium-scalestructure(onscalesoftensofthousandstohundredsofthousandsofkilometers)movingatspeedscomparabletothatoftheslowsolarwind. Thesestructureswereassociatedwithsignificantmagneticfieldrotationintheinterplanetarymedium, andappeartobeclosedorquasi-closedloop-likefeatures. Wediscusstheseobservationsintermsofthelighttheycastonslowwindstructure, andpresentawidersetofslowwindobservationswhereweinvestigatethepresenceofsmall- andmedium-scaleirregularitiesasacomponentofslowwindoutflow.
AnomalousSolarCyclesandtheEvolutionofCoronalHoles
BarbaraBromage (JeremiahHorrocksInstitute,UCLan)with Steven Chapman
A summaryoftheanomalousbehaviourofsolarcycle23iscomparedwiththatofthe15-yearcycle(cycle4)attheendofthe18thcentury. Ameansolarcycleisderivedandusedtocomparethecharacteristicsofthiscyclewithcycle23. Forexample, bothexhibittimeswhentheirevolutiondepartsfromthatofthemeancyclefor2or3years; priortothat, bothappeartoexhibitaphaseshiftofabouthalfasolarcycleinadvanceofaregular11-yearcycle(beginningwithzeroshiftatcycle1). SOHO-CDS synopticdatahavebeenusedtostudytheevolutionofcoronalholesthroughoutcycle23, atthesametimederivingthevariationintotalopenflux. In1998, thetwohemispheresdevelopedalagofabout2years,whichcanbeseentoleadtoadelayinthestartofthenextsunspotcycle, resultinginanextendedsolarminimum. Aswellaspredictingthenew-cyclestart, thedatasuggestthatcycle24willbeweak, lastinglongerthanthetypical11years.
ChiantiPy- A PythonInterfacetoCHIANTIKenDere (GeorgeMasonUniversity)
Pythonisafree, modern, object-orientedprogramminglanguagethatiswellsuitedtoscientificdataanalysis. A commandlineversionforusewithinaPythonshellisunderdevelopmentandwillbereleasedinthenearfuture.Programmatically, eachionintheCHIANTIdatabaseistreatedasanobject, providingagoodmatchtothestructureoftheCHIANTI database.ForanyionintheCHIANTI database, ChiantiPyisabletocalculateandplotlevelpopulations,spectrallineemissivities, contributionfunctions,G(n, T ), free-freeandfree-boundcontinua, andlineintensityratiosasfunctionsoftemperatureandelectronandprotondensity.
A pre-releaseversioncanbefoundathttp://sourceforge.net/projects/chiantipyandthecurrentdocumentationathttp://chiantipy.sourceforge.net.
RapidOscillationsintheSolarAtmosphereGarethDorrian (Queen'sUniversityofBelfast)with D.B. Jess, M. Mathioudakis, D.J. Christian,
F.P. Keenan, R.S.I. Ryans, and P.J. Crockett
RapidOscillationsintheSolarAtmosphere(ROSA) isahigh-cadence, highresolutionimagingsystemforstudyingthedynamicsolaratmosphere.ROSA consistsofsixcameraswhichcanbetunedtoobserveatdifferentwavebandsextendingfromthenearinfra-redtothenearultra-violet. Thiscapabilityenableshigh-cadencecharacterisationofsolaratmosphericphenomenaatmanywavebandssimultaneously. TheROSA camerascantakeupto30framespersecondinfullchipmodeorupto200framespersecondinwindowedchipmode. AttachedtotheDunnSolarTelescopeatSacramentoPeak, NewMexico;ROSA isnowavailableasanopenuserinstrumentfortheUK solarphysicscommunity. Thisposterpresentsasummaryoftheinstrumentcapabiltiesandsomeearlyresultsfromobservingcampaigns.Amongtheearlyresultsarehigh-cadencemulti-wavebandobservationsofintergranularmagneticbrightpoints, activeregions, sunspots, andlimbobservationsofsolarprominencesandspicules.
P33–P34 87
Largeamplitudetransverseoscillationsinamulti-strandedEUV prominence, triggeredbytransient
disturbancesJenniferHarris (UniversityofWarwick)with
C. Foullon, V.M. Nakariakov, and E. Verwichte
WepresenttheanalysisoftwosuccessivetrainsoflargeamplitudetransverseoscillationsinanEUVprominence, observedontheNorth-Eastlimbon30July2005. Theoscillatorytrainsaretriggeredbytransientdisturbancesproducedbytwosuccessiveflares, whichoccurredabout10hoursapartinthesameremoteactiveregion(locatedjustnorthoftheequator, around500Mmfromtheprominence). WeusetheSOHO/EIT 195 Aimageswitha12minutecadencetocompareoscillatorypropertiesspatially, indifferentstrandsoftheprominence, andbetweenthetwosuccessivelyexcitedoscillatorytrains. Theevolutionoftheprominence'sapparentheightabovethelimbisdeterminedusing304/195 AimageratiosfromSOHO/EIT,andthiscorrectionisappliedtoaccountforthesolarrotation. Thevariousfilamentarystrandsareseentoexhibitdifferentoscillatorybehaviour, intermsoftheiramplitudes,phasesandperiods. Thelargestamplitudes, whichoccurattheprominenceapex, areover20km/sforthefirstoscillatorytrainandaround5km/sforthesecond, whiletheperiodatthislocationisapproximately90minutesinbothcases. Somestrandsshowdecayingoscillationswithadecaytimeofabout6hours, whileoscillationsofotherstrandsaredecaylessandlastforsevencycles. Wediscusshowtheobservationsmayshedlightonthenatureoftheoscillationsandthetriggeringmechanism.
TheMagneticPropertiesofFlaringActiveRegionsPaulHiggins (TrinityCollegeDublin)with
PeterT. Gallagher, D. ShaunBloomfield, andR.T. JamesMcAteer
TheSolarMonitorActiveRegionTracking(SMART)algorithmisanautomatedsystemfordetecting,tracking, andcatalogingmagneticfeaturesthroughouttheirevolutionanddecay. TheSMARTmethodwillformthebasisofactiveregionextractionandtrackingwithintheHeliophysicsIntegratedObservatory(HELIO).Magneticpropertiessuchastotalflux, fluximbalance, fluxemergencerate, Schrijver'sR-value, R*(amodifiedversionofR),andFalconer'smeasurementofnon-potentialityaredeterminedforindividualfeaturesthroughoutsolarcycle23.SolarflaresmeasuredbytheGOES andHSIinstrumentsareassociatedwithdetectedfeatures,andtherelationshipbetweenflaresizeandmagneticpropertyvalueispresented.
HardX-RayStructureofLoopFootpointsinaSolarLimbFlare
EduardKontar (UniversityofGlasgow)withNatasha Jeffrey, Iain Hannah, and Marina Battaglia
Weapplynewly-developedX-rayvisibilityforwardfittingtechniquetoRHESSI dataofawell-observedlimbflaretoinvestigatetheenergyandheightdependenceonsizes, shapes, andpositionofhardX-rayfootpointsources. Thepositions, theverticalextentsandthewidthsofhardX-raysourcesaremeasuredasafunctionofenergy. Ourobservationssuggestthattheverticalandhorizontalsizesoffootpointsaredecreasingwithenergywhilehigherenergyemissionoriginatesprogressivelydeeperinthechromosphere. ThecharacteristicwidthsofthehardX-rayfootpointsourcealongthelimbdecreasewithheightandareconsistentwithaconvergingmagneticfieldin
thefootpoint. TheverticalsizesofX-raysourcesarelargerthanpredictedbycollisionalthick-targettransportinasingledensityscaleheightchromospherebutcanbeexplainedusingamulti-threadeddensitystructureoftheloop.
NewsolarprominencediagnosticswithEIS/Hinode
NicolasLabrosse (UniversityofGlasgow)withB. Schmieder, and P. Heinzel
ObservationsofasolarprominenceobtainedwiththeExtremeUltravioletImagingSpectrometer(EIS)onHinodeareanalysed. TheobserveddecreaseinbrightnessofEUV coronallinescanbeduetotwobasicmechanisms: absorptionandemissivityblocking. TheabsorptionofcoronallineradiationinEUV isduetothephotoionisationofhydrogen,neutralandionizedhelium. Thesecondmechanismisthevolumeblocking, duetothepresenceofcoolplasma, oroflowdensityhotplasma(cavity). WeillustratethesemechanismsusingseveralEIS spectralwindows, andconcentrateontherasterat256A whichcontainstheHeII lineblendedwiththreeothercoronallines. Wepresentatechniquetoremovetheblendbetweentheselines, takingintoaccounttheabsorptionandemissivityblockingofthecoronallines, toretrievethetrueHeII lineprofileinordertomakeadiagnosticoftheplasmaindifferentpartsoftheprominence.
KineticAlfvénwavesandprotonvelocitydistributioninthesolarwind
XingLi (AberystwythUniversity)
Observationsofthesolarwindhaveshownthatprotonvelocitydistributionfunctionshavedistinctiveshapes: inthefastsolarwindtheprotontemperatureinthedirectionperpendiculartothebackgroundinterplanetarymagneticfieldishigherthanintheparalleldirection. Thissuggeststhatacontinuousheatingmechanismisneeded. ThecurrentunderstandingofincompressibleMHDturbulenceincreasinglypointstotheimportanceofkineticAlfvénwaves. Astheenergyatlargescalesisconvertedtosmallerscales, MHDturbulencetheorydictatesthattheturbulentwavenumberwillincreaseintheperpendiculardirectionwhiletheparallelwavenumberislargelyunchanged. WeinvestigatetheeffectofkineticAlfvénwavesonthevelocitydistributionfunctionsofprotonsinthesolarwind. FirstweuselinearVlasovtheorytoobtainthepropertyofkineticAlfvénwaves. Thesewavespropagateinthedirectionalmostperpendiculartothebackgroundmagneticfield. Wethennumericallysimulatehowthesewaveswillheatprotonsandshapetheprotonvelocitydistributionfunctions. Atalmostperpendiculardirection, wavesareusuallyregardedasnearelectrostatic. However, wewillshowthatthemagneticfieldofthesewavescannotbeneglected.
Simulationsofmagneticfluxemergencewithanoverlyingfield
DavidMacTaggart (StAndrews)with A.W. Hood
MHD simulationsoffluxemergenceallowonetomodelthelarge-scalestructureofthedynamicevolutionofactiveregions. Modelsthatincludeanoverlyingmagneticfield, fortheemergingfieldtointeractwith, allowforthepossibilityofinterestingphenomena, suchasCME initiation. Inthistalkwewillconsidersomeoftheseeffectsanddiscusstheirimplications.
Phasemixingofnon-linearAlfvénwavesJamesMcLaughlin (NorthumbriaUniversity)with
I. DeMoortel, and A.W. Hood
Weconsiderthebehaviourofnon-linear, non-idealAlfvénwavepropagationwithinaninhomogeneousenvironmentinboth1D and2Dandfindclearevidencefortheponderomotiveeffectandvisco-resistiveheating. TheponderomotiveeffectgeneratesalongitudinalcomponenttothetransverseAlfvénwave–withafrequencytwicethatofthedrivingfrequency.Analyticalworkshowstheadditionofresistiveheating. Thisleadstoasubstantialincreaseinthelocaltemperatureandthusthermalpressureoftheplasma, resultinginmaterialbeingpushedalongthemagneticfield. ConsideringAlfvénwavepropagationin2D withaninhomogeneousdensitygradient, wefindthattheequilibriumdensityprofileissignificantlymodifiedbyboththeflowofdensityduetovisco-resistiveheatingandthenon-linearresponsetothelocalisedheatingthroughphasemixing.
SDO/AIA responsetocoronalhole, quietsun,activeregionandflareplasma
BrendanO'Dwyer (UniversityofCambridge)withHelen Mason, and GiulioDel Zanna
WeexaminethecontributionofspectrallinesandcontinuumemissiontothechannelsoftheAtmosphericImagingAssembly(AIA) ontheSolarDynamicsObservatory(SDO) indifferentregionsofthesolarcorona. Syntheticspectrawereobtainedusingsampledifferentialemissionmeasures(DEM) forcoronalhole, quietsun, activeregionandflareplasma. Thesesyntheticspectrawereconvolvedwiththeeffectiveareaofeachchannel, inordertodeterminethedominatecontributionindifferentregionsofthesolarcorona. WehighlightthecontributionofparticularspectrallineswhichundercertainconditionscandramaticallyaffecttheinterpretationofSDO/AIAdata.
Alfvénwavephase-mixinganddampingintheioncyclotronrangeoffrequencies
JamesThrelfall (UniversityofStAndrews)withI. DeMoortel, and K.G. McClements
ThephasemixingofshearAlfvénwaveshasbeenproposedasamechanismforsolarcoronalheating[1]andsuchwavesmayalsoplayanimportantroleinflareheatingandparticleacceleration[2].Anytreatmentofshear-AlfvénwaveswithfrequenciesthatareasignificantfractionoftheiongyrofrequencymusttakeintoaccounttheHallterminthegeneralisedOhm'slaw. Weuseanumericalscheme, Lare2D,toinvestigatehowthephase-mixinganddampingofashear-AlfvénwaveareaffectedbytheinclusionoftheHallterm,whichsplitsitintoaleft-circularlypolarisedioncyclotronwaveandaright-circularlypolarisedwhistlerwave. Thepresenceofatransversegradientinwavepropagationspeedcauseswavedampingtooccurviaphase-mixing(HeyvaertsandPriest[1]), whichcanbeaffectedbythedispersivepropertiesoftheioncyclotronandwhistlerwaves.RunningLare2D forthecaseofasinglesmallamplitudeperturbation, wehaverecoveredresultsobtainedbyHoodet. al. [3]intheMHD limit.WearenowusingthecodetomodelthedampingofsuchapulseintheHall-MHD regime, andinthepresenceofequilibriumgradients.
ThisworkwasfundedbytheEngineeringandPhysicalSciencesResearchCouncil, throughaCASE awardandgrantEP/G003955, andbythe
88 P34
EuropeanCommunities, underthecontractofAssociationbetweenEURATOM andCCFE.TheviewsandopinionsexpressedhereindonotnecessarilyreflectthoseoftheEuropeanCommission.
[1]Heyvaerts, J.andPriest, E.R., Astron.Astrophys. 117, 220(1983)[2]McClements, K.G.andFletcher, L., Astrophys. J.693, 1494(2009)[3]Hood, A.W., Brooks, S.J., andWright, A.N.,Proc. R.Soc. Lond. A,458, 2307(2002)
AutomateddetectionandtrackingofmagneticfragmentsindecayingsolaractiveregionsFraserWatson (UniversityofGlasgow)with
Lyndsay Fletcher
Thebreakupanddecayofsolaractiveregionsisaprocessthatiscurrentlynotwellunderstood. Toprovidemoreinsightintothenatureofthedecay,wehavedevisedamethodforautomaticallydetectingmagneticfragmentswithinactiveregionsandtrackingthemthroughmultipleimages. Thisisdoneusing96minutemagnetogramstakenbytheMDI instrumentonboardSOHO andgivesus13yearsofconsistentdatatoworkwith. A catalogueofactiveregionfragmentshasbeencompletedfortheyear2001, duringthepeakofthelastsolarcycle, andhasallowedustolookatphysicalpropertiesoftheindividualfragments, tracktheirpositionand'propermotion'andexaminetheoverallfragmentdistributions. Wehopetousethecataloguetodeterminepossiblecausesofactiveregionbreakupandlookforanytrendsthatexistinthisprocess. I willpresenttheresultsofthispreliminaryanalysisofthe117,242fragmentsdetected, alongwithsomeideasforfutureuseofthealgorithmsandcatalogue.
P35FIRST Explorer- spacebornelow-frequencyradio
astronomyusingpassiveformationflyingJanBergman (SwedishInstituteofSpacePhysics)
with Richard Blott, Alistair Forbes,David Humphreys, David Robinsson, and
Constantinos Stavrinidis
Space-bornelow-frequencyradioastronomyhasbeenidentifiedasakeyscienceapplicationforaconceptualpathfindermission, usinganovelspace-flightconceptcalled“passiveformationflying”. Themission, FIRST Explorer(Formation-flyingsub-IonosphericRadioastronomyScienceandTechnology), iscurrentlyunderstudybytheEuropeanSpaceAgency(ESA).Itsobjectiveistodemonstratepassiveformation-flyingandtoperformuniquesciencewithaveryhighserendipityfactor, byopeninganewfrequencywindowtoastronomy. Traditionally, formation-flyingrequirescontinuousandminutecorrectionsoftheorbitalelementsandattitudesofthespacecraft. Thisincreasesthecomplexity, andassociatedrisk, ofcontrollingtheformation, whichoftenmakessuchstudiesinfeasiblefortechnologicalandeconomicreasons. Passiveformation-flyingoffersaremedytothoseproblems. Spacecraftinapassiveformationareallowedtodriftandrotateslowly, butbyusingadvancedmetrologyandstatisticalmodellingmethods, theirrelativepositions, velocities, andorientationsaredeterminedwithveryhighaccuracy. Themetrologydataisuseddirectlybytheradioastronomypayloadtocompensateforspacecraftmotionsinsoftware. Thenormallyverystringentspacecraftcontrolrequirementsare
therebyrelaxed, whichsignificantlyreducesmissioncomplexityandcost.
Hydroxidecatalysisbondingresearchforastronomicalapplications
NicolaBeveridge (UniversityofGlasgow)
TheInstituteforGravitationalResearchattheUniversityofGlasgowhasawellestablishedhistoryintheresearchofhydroxidecatalysisbondingforgroundandspacebasedgravitationalwavedetectorapplications. Hydroxidecatalysisbonding, usedtobondsilicasuspensionelementstosilicamirrorsandforbondingsilicaopticstoZerodur, producesstrong, thermallyconductiveandlowlossbonds. Thetechniquecanbeappliedtomanyother(oxide)materialsandisthereforeofinterestforalternativepurposes, includingastronomicalprojectssuchastheExtremelyLargeTelescopewherePZT materialisbondedtosiliconorsiliconcarbide, oropticalfilterapplicationswherecoatedsilicasubstratestocanbebondedontosilicadiscsinordertotransfercoatings. Thispresentationisaimedatgivingabriefoverviewoftheresearchofafewoftheseapplications.
HARMONI - A UK ledfirstlightspectrographfortheE-ELT
FraserClarke (UniversityofOxford)withNiranjan Thatte(PI)
HARMONI isavisible/near-infraredintegralfieldspectrographcurrentlybeingconsideredasoneofthefirstlightinstrumentsforthe42-mEuropeanExtremelyLargeTelescope. HARMONI willprovidemedium-highresolution(R∼ 5000 − 20000)spectroscopyintheV-Kbands(0.47-2.5microns)overanextendedfieldofupto10x5arcseconds. Itwillprovidearangeofpixelsscalesof40mas/pixeltosamplethetelescope'sGLAO correctedPSF,downto4mas/pixeltosamplethediffractionlimitedimagesprovidedbytheATLAS-LTAO system.
I willoutlinethekeysciencecasesforHARMONI,rangingfromextrasolarplanetstohighredshiftgalaxies, alongwiththekeytechnologieswhichwillmakeHARMONI possible.
TheHARMONI consortiumisUK-led(UniversityofOxfordandUKATC),withFrenchandSpanishpartners, andoffersthepossibilityofkeyUKinvolvementintheE-ELT attheveryearliestopportunity. Alongwith7otherinstruments,HARMONI hasrecentlycompletedaphaseAconceptualstudyforESO.
LumpedElementKineticInductanceDetectorssuitableforlargearraysofastronomical
detectors.SimonDoyle (CardiffUNiversity)with
Phil Mauskopf
TheLumpedElementKineticInductanceDetector(LEKID) isasimpletofabricate, superconductingdevicesuitableforuseinlargemultiplexeddetectorarrays. TodatetheLEKID hasdemonstrated200microndetectionofacryogenicblackbodysourceandsuccessfultestingofademonstrationarrayoperatingat2mmontheIRAM telescopeinOctober2009. DuetoitscombinedabsorbinganddetectingelementstheLEKID isanextremelysimpledetectortofabricaterequiringonlyonedepositionandetchsteptoproduceanarrayofupto1000pixelsbeingmultiplexedontoasinglefeed-line. TheLEKID isalsoaverycompactdetectormakingitidealforproducingarrayswithhighfillingfactors. The
suitabilityoftheLEKID foruseinlargearrayshaspromptedareturnvisittotheIRAM telescopewithadualbandinstrumentin2010. ThispresentationwillgiveanoverviewoftheLEKID detectoraswellasitsuseoutsidethemmandsubmmastronomybands.
Milli-kelvincoolerfortheXMS instrumentontheInternationalX-rayObservatory
IanHepburn (UniversityCollegeLondon–MSSL)
Theworldsfirstcryogenfreeflightworthyadiabaticdemagnetisationrefrigeratorforthecoolingofcryogenicdetectorsto50mK wasdeliveredtoESA inJune2008. ThissystemwasdevelopedbyMSSL inassociationwithEADSAstriumundercontracttoESA anddevelopedasatechnologydevelopmentfortheXEUS mission(nowrenamedtheIXO).TheADR wasconstructedasasetofsub-systemsinordertoenablechangesintechnologyandrequirementsatalaterdatetobeintegratedintothesystem. Vibrationqualificationwasperformedonthesub-systemstoAriane5levels.
InthispresentationwepresentdetailsofthedeliveredADR,itssub-systems, theproposed50mK coolerforthecoolingoftheTES detectorsontheX-raymicrocalorimeterspectrometerinstrument(XMS) fortheInternationalX-rayobservatoryandongoingdevelopmentinheatswitchtechnologywhichwillenableacontinuousADR tobeconstructed.
High-PrecisionInterferometryandLow-LossmaterialsforfutureGravitationalWave
ObservatoriesStefanHild (UniversityofGlasgow)
Large-scaleMichelsoninterferometersformthecoreofcurrentandfutureGravitationalWaveAntennas. SincethedaysofAlbertMichelsonandEdwardMorley, thesensitivityofMichelsoninterferometershasbeenimprovedbymorethan12ordersofmagnitude. Tofurtherimproveourabilitytoscantheskyforgravitationalwavesignalsavarietyofinnovativeinterferometrictechniquesandlowlossmaterialsarerequired. Thiswillleadto2ndand3rdgenerationdetectorssuchasAdvancedLIGO andtheEinsteinTelescope.
Thistalkwillsurveycurrent/futuretechniquesininterferometrysuchassqueezedlight, opticalrigidityandotherQuantum-Non-Demolitiontechniques. Furthermore, thepropertiesofSiliconasacryogenicmaterialandthenovelconceptofamonolithicreflectorbasedonmicro-structuredsurfaceswillalsobepresented. Thisallowsthefabricationofhighlyreflectivemirrorswithouttheuseofdifferentmaterials, whichresultsisanopticalcomponentwithalowthermalnoise.
Reducingriskincryogenicinstrumentdesign:thermalconductivitymeasurementsattheCryogenicInstrumentationResearchLab
JuliaKennedy (InstituteforAstronomy, UniversityofEdinburgh)with A.L. Woodcraft
Poorknowledgeofthephysicalpropertiesofmaterialsisaseverelimitationoncryogenicdesign, andasinstrumentsincreaseincomplexitywhilebudgetsshrinkthislackofknowledgeisposinganincreasingrisktocostsandschedules.
Furthermoremanynewmaterials, particularlypolymers, offertheprospectofimprovedperformancebutthereislittleinformationontheircryogenicproperties.
P34–P35 89
Unfortunately, veryfewgroupscapableofmakingusefulmeasurementsareabletodevotesignificanttimetodoingso. AttheCIRL (CryogenicInstrumentationResearchLaboratory), wearecarryingoutasystematicprogrammeofmeasurementsofthethermalandelectricalpropertiesofmaterialsfrombelow4K toroomtemperature, concentratingonthoseofuseinlargecryogenicinstruments.
ThesemeasurementsarepartofaUK governmentfundedprogrammetoimprovetheabilitytoconstructcryogenicinstrumentsinbothacademiaandindustry.
Wepresenttheresultsofinitialmeasurementsanddiscussourplansforthenearandlonger-termfuture.
NoveldeformablemirrordevelopmentsforastronomyapplicationsMelStrachan (UKATC)
TheUKATC hasbeencollaboratingisaseriesofprojectsdirectedtowardsaddressingtheadaptiveopticchallengesposedbytheEuropeanExtremelylargetelescope. Wehavedevelopednoveltechnologicalsolutionsforbothlargedeformablemirrorsfortelescopewavefrontcorrection, andminiaturedeformablemirrorsforusewithininstruments. Ourlargedeformablemirrorsurfacematerial, acompliantfromofsiliconcarbide,offersaYoung'sModuluscomparabletoglassbutwithgreater, non-catastrophic, resistancetofracture. Incombinationwiththeextraordinarynewmaterialwehavebeenworkingonanewlow
poweractuatorwithadeflectioncapabilityoftensofmicrons.
AdaptiveopticrequirementsforinstrumentationsuchasEAGLE fortheEuropeanextremelylargetelescopepresentanenormouschallengetodeformablemirrortechnology. Wehavedevelopedauniqueapproachusingfabricatedarraysofmultilayeractuatortechnologytoaddresstherequirementsofactuatordensityanddeflection. Ourprogrammeofworkhasuncoveredanovelapproachwhichhasledtoabuiltintestcapability. Wewillpresenttheoutcomesofourworkwhichwebelievewillleadtoacompactdeformablemirror.
Probingtheatmospheresofextrasolarworldswithadedicatedmissionfromspace
GiovannaTinetti (UCL) with M. Swain,M. Tessenyi, M. Ollivier, G. Vasisht, P. Deroo,J.P. Beaulieu, T. Henning, and THESIS team
TheTHESIS missionconceptisaspace-based,modestcost, lowtechnicalriskmissioncapableofcharacterizingtheatmospheresofexoplanets,includingsuper-Earthsinthehabitablezone.Significantly, THESIS doesnotrequirenewtechnology. BuildingonthesuccessesoftheSpitzerandHubblespacetelescopes, THESISwouldbehighlyoptimizedforsystemstability(1partin 105)andwoulddeliverphoton-noise-limitedspectroscopyandphotometryoverthecrucial0.5–16micronwavelengthrange. Thisrangeofwavelengthscontainssignaturesofwater,methane, ammonia, carbonmonoxide, andnumerousothermolecules, andincludesmoleculesofpotentialprebioticsignificance.
Becausemoleculesserveasprobesofcomposition, conditions, andchemistry, molecularspectroscopyofthedaysideandnightsideregionsofexoplanetatmospheresisthemostpowerfultoolavailableforstudyingtheseobjects. THESISwouldbethefirstmissionexplicitlydesignedtocharacterizeplanetswherelifecouldexist; THESISwouldprofoundlyadvanceourunderstandingofthephysicalconditionsandlikelythehistoriesofexoplanets, rangingfromhot-Jovianstosuper-Earths. THESIS wouldbealow-costUS-Europeanmissionwithenormousdiscoverypotential.
Astronomyatthehighestenergies: theCherenkovTelescopeArray
RichardWhite (UniversityofLeeds)
Very-HighEnergy(VHE) γ−rayastronomyisdominatedbyImagingAtmosphericCherenkovTelescopes(IACTs)andisreliantuponthedetectionofCherenkovradiationfromelectronsincascadesinitiatedbyastrophysical γ−rayshighintheEarth'satmosphere. Resultsfromthelatestgenerationoftelescopes, suchasHESS,MAGICandVERITAS haverevealedaskyrichwithdifferentclassesofVHE object.
StillthelimitsoftheIACT havenotyetbeenreached, andtopushthehigh-energyfrontierofphotonastronomytheCherenkovTelescopeArray(CTA) hasbeenproposed. Comprising50-100IACTsoftwotothreesizes, CTA willprovideanorderofmagnitudeincreaseinsensitivityfrom∼ 3 × 1010 to ∼ 1014 eV.Despitetheextremeenergies, CTA willpossessthebestsensitivityandangularresolutionatanyenergyabovethehardX-rayband.
90
Inde
x of
Aut
hors
Abdulgalil, Ali, 63Achilleos, N., 52Achilleos, Nicholas, 52, 58Agalya, G., 75Agueda, Neus, 68Aguilar-Rodriguez, E., 75Aird, James, 84Akeson, R., 73Al-Salti, Nasser, 59Alexander, C., 54, 85Alexander, Caroline, 48ALFALFA Team, 44Allard, France, 51Allende-Prieto, Carlos, 45Almaini, Omar, 82Anderson, J.P., 46Andrews, D.J., 67Andrews, David, 65Antonova, A.E., 52Arce, H., 63Archontis, Vasilis, 87Argiroffi, C., 84Argo, Megan, 71Arridge, C.S., 58, 66Arridge, Chris, 51, 66Aruliah, A.L., 67Asai, A., 80Aschwanden, M.J., 81ASPERA team, 59Austin, Matthew, 45Avison, Adam, 45Awad, Zainab, 64Aylward, Alan, 79
Bacon, D.J., 50Baddeley, L., 67Badnell, N.R., 80Bagheri, Gemma, 61Bagnulo, Stefano, 84Bailin, Jeremy, 84Baillie, Orsolya, 65Bains, Indra, 73Bains, William, 42Baker, D., 81Baker, Deb, 54Baker, Deborah, 48Baker, Jo, 83Bakunina, I.A., 60Baldry, Ivan, 76Baldry, IvanK., 45Ballai, I., 61Ballai, Istvan, 60Balogh, Andre, 59Barclay, Charles, 85Bareford, Michael, 73Barker, Michael, 78Barlow, M., 51Barlow, MichaelJ., 58Barnsley, Robert, 49Baron, F., 73Baron, Fabien, 72Barr, Ewan, 81Barstow, M.A., 58Basa, S., 57Bassett, B., 77Battaglia, Marina, 68, 88Baugh, C.M., 63Bayet, Estelle, 64, 64, 65Beaulieu, J.P., 90Beggan, C., 79Beggan, Ciaran, 65Benisty, Myriam, 72Bennet, Euan, 58Benson, A., 57Benson, A.J., 63Benson, Kevin, 75Bentley, Robert, 75Bento, Joao, 49
Berger, J.P., 72Bergman, Jan, 89Bernard, J.-P., 78Best, P.N., 44Best, Philip, 44, 63Beswick, R.J., 50Beswick, Rob, 71Beveridge, Nicola, 89Bewsher, D., 54, 81Bewsher, Danielle, 52, 85Bian, Nicolas, 68Bibby, Joanne, 45Bingham, R., 59, 70Binks, A., 73Birch, M.J., 79Birkinshaw, M., 83Bisi, Mario, 75, 87Blake, R., 61Blake, Rob, 54, 62Blanc, AnjaLe, 75Blott, Richard, 89Bluck, Asa, 82Bonfield, Dave, 62Borg, A., 47Bouvier, J., 84Bower, Richard, 77Bradshaw, S.J., 80Bradshaw, Steve, 79Braidwood, L., 48Breen, A.R., 75, 87Bretherton, Claire, 86Brockley-Blatt, C., 54Bromage, B.J.I., 54, 79Bromage, Barbara, 87Brook, C.B., 83Brook, Chris, 56, 84Brook, ChrisB., 45, 84Brooke, John, 54, 75Brookes, Mairi, 63Brown, D.S., 52, 54, 85Brown, John, 68, 70Browne, Ian, 44Browning, P.K., 68Browning, Philippa, 68, 73Brunner, RobertJ., 77Bruno, R., 54Brunthaler, Andreas, 71Bryan, Sarah, 83Buckle, Jane, 46Buffington, A., 75Bulger, J., 84Bulger, Joanna, 63Bunce, E.J., 66Bunclark, Peter, 62Burge, Christina, 68Burke, Claire, 43Burningham, Ben, 77Buscher, D., 73Buscher, David, 72, 72Butters, Oliver, 55Byrne, JasonP., 75
Cairns, R.A., 59, 70Calura, Francesco, 84Cameron, A.C., 55Cameron, Andrew, 42Cameron, AndrewCollier, 73Cameron, Ewan, 44Campusano, L.E., 83Cano, Zach, 70Caputi, Karina, 62Cardoso, Catia, 51Cargill, Peter, 79Carlberg, R., 57Carozzi, Tobia, 55Carpenter, J., 63Carpineti, Alfredo, 43Carr, C.M., 53
91
Carr, Chris, 53Caswell, James, 45Cayless, Alan, 55Cecconi, B., 52Cernicharo, J., 51CFHTLenS team, 72Chaizy, P.A., 47Chaplin, W., 86Chapman, S.A., 54Chapman, S.C., 47Chapman, Sean, 64Chapman, Steven, 87Charalambous, A., 67Charnley, Steven, 64Chashei, I.V., 75Che, Xiao, 72Chesneau, Olivier, 72Chiavassa, A., 73Chisham, G., 53Chorley, Nicky, 60Christian, D.J., 87Christian, Damian, 60Christie, Helen, 64Christodoulou, Leonidas, 43Christopher, Natalie, 64Churcher, Laura, 51Cilliers, P., 67Cioni, Maria-Rosa, 61, 61, 62, 79Clark, J.S., 46Clark, James, 82Clark, Simon, 46Clarke, Ellen, 65Clarke, Fraser, 89Clarke, J.T., 52Clementini, Gisella, 62Clements, D.L., 50Clements, David, 49Clilverd, Mark, 65Clover, J.M., 75Clowes, R.G., 83Coates, A.J., 52, 66Coates, Andrew, 66Cole, S., 63Collings, MarkP., 64Collins, C., 43Collins, Ross, 54, 61, 62Colombi, Stephane, 56Conley, A., 57Conselice, Christopher, 82Contursi, A., 64Cooper, Heather, 46Coppin, K., 44Corder, S., 63Cormier, Diane, 64Couchman, Hugh, 84Courty, S., 83Cowley, S.W.H., 52, 65--67Cran-McGreehin, A.P., 70Creech-Eakman, M., 73Crockett, P.J., 87Crockett, Philip, 60, 60Crooker, Nancy, 75Cross, A.W., 59, 70Cross, N., 61Cross, Nicholas, 62Cross, Nick, 54Crothers, S., 53Crowther, Paul, 45Culhane, Len, 48, 54Cunningham, Colin, 42CurtisLake, Emma, 44
daCosta, A.A., 81daCosta, AntonioArmando, 82Dai, Y., 69Dall'Ora, Massimo, 62Dalla, S., 54, 85Dalla, Silvia, 68
Dalton, Gavin, 44Dandouras, I., 47Dandouras, Iannis, 46Darling, Jeremy, 44Dasso, S., 75Davies, B., 46Davies, Ben, 46Davies, J.A., 47, 53, 59, 75, 76, 87Davis, C.J., 59, 76Davis, Chris, 75Davis, Christopher, 75Davis, Gary, 49Davis, Olaf, 56Davs, C.J., 53Dawson, Ewan, 65Day-Jones, Avril, 77DeMoortel, I., 61, 88DeRosa, Robert, 84Deane, Roger, 63DEBRIS consortium, 51Decin, L., 51DeJong, J., 64DelZanna, G., 48, 80DelZanna, Giulio, 48Demoulin, P., 75, 81Demoulin, Pascal, 74DePasquale, Massimiliano, 70Dere, Ken, 87Deroo, P., 90Devriendt, Julien, 56, 83Diamond, Phil, 73Dickinson, Mark, 82Dickson, Ewan, 68Dilday, B., 77Dimbylow, T.G., 47Ding, Jiaoyang, 80Diver, D.A., 82Diver, Declan, 80, 81Diver, DeclanA., 58, 80Dominguez, SantiagoVargas, 48Donati, J.-F., 84Donati, Jean-Francois, 73Dorrian, G.D., 87Dorrian, Gareth, 87Dougherty, M.K., 66, 67Dougherty, Michele, 53Dougherty., M.K., 52Down, Emily, 83Doyle, Gerry, 51Doyle, J.G., 52, 76, 80, 81Doyle, Simon, 89Driel-Gesztelyi, Lidiavan, 74Driver, Simon, 44Dufour, P., 58Dunlop, J.S., 44Dunlop, James, 62Dunlop, Jim, 63Dunlop, M.W., 47Duthie, Roger, 46
e-MERGE consortium, 63Eastwood, Jonathan, 47Edberg, N.J.T., 67Efstathiou, George, 42Egami, E., 56Eke, V.R., 57Eldridge, John, 78Ellis, Richard, 78Elsworth, Y., 86Emerson, Jim, 62Erdélyi, R., 60, 61, 86ESA,50Escoubet, C.Philippe, 47Escoubet, C.P., 47Espinoza, Cristobal, 81Evans, A., 46Evans, Christopher, 46Evans, D.A., 83
Eyles, C.J., 52, 53Eymeren, Janinevan, 71Eyres, S.P.S., 46
Falcke, H., 50Falder, James, 83Fallows, R.A., 75, 87Famaey, Benoit, 72, 84Farihi, Jay, 58Fazakerley, A.N., 47, 48, 54, 76Fazakerley, Andrew, 46Fear, Robert, 74Fedeli, Cosimo, 71Feigelson, E.D., 84Feix, Martin, 71, 72, 84Fender, R., 50Fenech, Danielle, 71Ferdman, Robert, 82Ferguson, A., 78FermiGBM Collaboration, 70Ferreras, Ignacio, 44, 56, 78Findlay, Joseph, 62Finger, Lars, 63Fischer, J., 64Flaccomio, E., 84Fletcher, Lyndsay, 48, 69, 80, 89Fludra, Andrzej, 53, 53FMOS team, 44Folsom, C., 84Forbes, Alistair, 89Forgan, Duncan, 55Fornacon, K-H., 47Forsyth, C., 47, 48Forsyth, Colin, 47Forsyth, RobertJ., 59Fossati, L., 84Fouchez, D., 57Foullon, C., 88Frankland, Victoria, 64Franz, M., 67Fraser, Morgan, 70Freeman, M.P., 53Frenk, C.S., 63Frenk, Carlos, 56Freytag, B., 73Fujihara, Gary, 86Fujiki, K., 75Fullekrug, Martin, 66Fuller, G,50Fuller, Gary, 45, 64, 64, 65
Gerard, J.-C., 52Gaensicke, Boris, 76GalaxyZooteam, 43, 55GALEX Collaboration, 78Gallagher, Peter, 75Gallagher, PeterT., 88Galsgaard, K., 74, 80Galsgaard, Klaus, 74GAMA Team, 43--45Garrett, M., 50Garrington, Simon, 49, 71Garza, K., 47Gaunt, C.T., 67Geach, Jim, 44, 77Geballe, T.R., 46Geen, Sam, 83Gentile, Gianfranco, 72Genzel, R., 64Getman, K.V., 84Ghodsi, Hoda, 56Gibson, B.K., 83Gibson, Brad, 84Gibson, BradK., 45Gillespie, K.M., 59, 70Gilmore, G., 57Giunta, A.S., 75Glubokova, S.K., 75
92
Goldstein, M., 47Gombosi, T.I., 85Gonzalez-Esparza, A., 75Gonzalez-Solares, Eduardo, 62GordonEmslie, A., 69Gordon, James, 72Gordon, K.D., 78Gordovskyy, Mykola, 68Gough, D., 86GraciaCarpio, J., 64Grady, Keith, 69, 69Graham, David, 48Graham, M.J., 83Grande, M., 59, 67Granot, Jonathan, 70Gray, Norman, 55Greaves, Jane, 51Green, James, 45Green, L.M., 85Green, Lucie, 48, 54, 85Green, LucieM., 74Gregory, Scott, 84Grey, Malcolm, 73Griffin, E.M., 67Griffin, Matt, 50Grocott, A., 47, 52Grocott, Adrian, 66Grocutt, Emma, 72Grodent, D., 52Guandalini, Roald, 62Guio, P., 52, 58Guo, Jingnan, 69Gupta, Jennifer, 44Gürkan, Gülay, 71
H-ATLAS team, 51Haas, M., 64Habergham, Stacey, 46Haberzettl, L., 83Hailey-Dunsheath, S., 64Haines, C., 56Hall, Elizabeth, 63Hallinan, G., 52Hallinan, Gregg, 51Hambly, N., 61Hambly, N.C., 58Hambly, Nigel, 54, 55, 62Hamilton-Morris, Victoria, 56Hammond, Giles, 85Hancock, B.K., 54Haniff, C., 73Haniff, C.A., 73Haniff, Chris, 72Hannah, Iain, 48, 68, 69, 88Hapgood, M.A., 47Hapgood, Mike, 47, 53, 75Hara, H., 48Hardcastle, M., 83Hargreaves, John, 79Harniman, R., 77Harper, Graham, 73Harra, L.K., 48, 76Harra, Louise, 54Harra, LouiseK., 49Harris, Jennifer, 88Harris, Kathryn, 83Harrison, Michael, 74Harrison, Richard, 53Harrison., R.A., 76Harvey, Janice, 86Hatchell, Jennifer, 42Haubois, X., 73Haynes, Andrew, 74He, W., 59Heald, George, 50Heavens, Alan, 72Hebden, Kerry, 64Heinke, CraigO., 82
Heinzel, P., 88Hellier, C., 42, 55Hempel, M,62Hendry, Martin, 57, 85Hendry, MartinA., 56, 57, 82Heng, IkSiong, 82Henning, T., 90Hepburn, Ian, 89HerMES Consortium, 51HerschelMESS Keyprojectconsortium, 58HESS Collaboration, 82HeViCS Consortium, 51Heyden, Kurtvander, 50Heyer, Inge, 86Heymans, Catherine, 72Heywood, Ian, 63Hick, P.P., 75HIFI consortium, 50Higgins, Paul, 88Hild, Stefan, 89Hill, David, 44, 44Hillier, Dan, 86Hnat, B., 47, 60Ho, Wynn, 82Hoare, M.G., 46Hodgkin, Simon, 62Hodgson, Lisa, 63Hoekstra, Henk, 71, 72Holliman, M., 61Holliman, M.S., 55Holliman, Mark, 54, 55Holme, Richard, 66Homeier, Derek, 51Honary, F., 67, 79Hood, A.W., 88Hood, Alan, 48Hood, AlanW,87Hook, I., 57Horbury, Tim, 75Horn, Markus, 57Horne, RichardB., 79Hornig, Gunnar, 74, 74House, Elisa, 83HowelI,V.S.C., 67Howell, D.A., 57Hoyle, B., 50Hsieh, Henry, 58Huang, Zhenghua, 80Hudson, Hugh, 60, 80Humphreys, David, 89Humphries, Thomas, 65Hussain, G.A.J., 84Hussain, Gaitee, 85Hutcheon, Richard, 78Hutchinson, James, 66Hutchinson, M.G., 47Huxor, Avon, 55, 77
Ibar, Edo, 44Ibata, R., 78Ibrahimov, M., 84Indebetouw, R., 78Inglis, A.R., 60Irwin, M., 78Irwin, Mike, 62Isella, A., 72Ivanov, V,62Ivison, R.J., 44Izzo, C., 84
Jackson, B.V., 75Jackson, Brendan, 57Jackson, Neal, 71Jackson, Richard, 85Jaffe, Andrew, 76Jain, R., 86Jain, Rekha, 74JamesMcAteer, R.T., 75, 88
James, P.A., 46James, PhilA., 45Jansari, Kishan, 61Jardine, M., 84Jardine, Moira, 52Jarvis, Matt, 50, 62, 83Jatenco-Pereira, V., 85Jeffrey, Natasha, 88Jeffries, Rob, 85Jensen, E.A., 75Jess, D.B., 87Jess, David, 60, 60JodcastTeam, 86John, Daniel, 57Johnson, Olivia, 86Johnston, Russell, 44Jones, Geraint, 59, 66Jones, GeraintH., 59Jones, Hugh, 77Jones, Mark, 55Jones, Olivia, 78Jonsson, Jakob, 57Josselin, E., 73Jurgenson, C., 73
Kanani, Sheila, 66Kataria, D.O., 54Kavanagh, A.J., 68Kaviraj, S., 43Kaviraj, Sugata, 78Kawata, Daisuke, 45Kay, ScottT., 83Keenan, F.P., 87Keenan, Francis, 60Kellett, B.J., 52, 59, 70Kellett, Stephanie, 66Kelly, Gemma, 66Kelly, J., 54, 85Kelvin, Lee, 44, 44Kemper, Ciska, 64Kemper, F., 78Kennedy, Grant, 51Kennedy, J., 75Kennedy, Julia, 89Keogh, Dominic, 82Ker, Louise, 63Khotyainstev, Yu. V., 47Kidd, Robert, 59Kiessling, Alina, 72Kim, Hansik, 63King, Robert, 51Kipping, David, 58Kirk, J.M., 51Kistler, L., 47Kitching, Tom, 72Kivelson, M.G., 52Kiyani, Khurom, 47Klaas, U., 64Klockner, Hans-Rainer, 63Kochukhov, O., 84Koda, J,63Kontar, E.P., 48, 69Kontar, Eduard, 68--70, 88Kosch, M., 67Kosch, M.J., 67Kotze, P., 67Kraemer, K.E., 78Kraft, R.P., 83Kramer, M., 82Kraus, Stefan, 72Krause, O., 64Kukula, Marek, 75, 86Kunawicz, Nadya, 65Kurtz, Donald, 86Kuznetsov, Alexey, 51
Laakso, H., 47Laatsch, Shawn, 86
93
Labrosse, Nicolas, 88Lacerda, Pedro, 58Lacey, C.G., 63Lagadec, E., 78Laing, E.W., 81, 82Laird, Elise, 82, 84Lampeitl, H., 77Lamy, L., 52, 65, 67Landstreet, J.D., 84Lang, Pauline, 52Langer, Norbert, 78LAT Collaboration, 70Lavraud, B., 47Lavraud, Benoit, 75Lawrence, Andy, 63Lawrie, Craig, 57LeBlanc, Anja, 54Leech, Jamie, 45Leier, Dominik, 78Leland, B., 84Lemke, D., 64Lester, M., 47, 66, 67Lester, Mark, 53, 66Levan, A., 71Levan, A.J., 71Levan, Andrew, 82Lewis, G., 78Lewis, Gethyn, 66Lewis, James, 62Li, Baojiu, 72Li, Chuan, 69Li, Xing, 88Liang, Guiyun, 80LIGO ScientificCollaboration, 71Lim, Jeremy, 73Lin, Bob, 42Linden, RonaldVander, 73Lindsey, C.A., 60Linker, J.A., 75Lintott, Chris, 55, 75Linz, H., 64Littlefair, Stuart, 52Liu, Siming, 69, 69Livi, S., 54LOFAR imagingcommissioningteam, 50Logue, Joshua, 57Lotz, S.I., 67Louarn, P., 54Loveday, Jon, 43, 77Lowe, Stuart, 86Lu, Q.M., 80Lucas, Philip, 62Lucek, E., 47Lucek, Elizabeth, 46, 53, 53Lui, A., 47Lumsden, S.L., 46Luna, Marialejandra, 60Lutz, D., 64Lykou, Foteini(Claire), 72Lyne, A., 82Lyne, A.G., 81
Maccio, Andrea, 72Macdonald, Erin, 44Macintosh, B., 84Mackay, D.H., 76, 80MacKinnon, A.L., 52MacKinnon, Alec, 68, 70, 86MacLachlan, CraigS., 80Maclean, R.C., 48Maclean, Rhona, 74MacTaggart, David, 88Madden, S., 64Madjarska, M.S., 76, 80, 81Madjarska, Maria, 80, 81Majewski, Pawel, 57Malbet, F., 72Mallik, Procheta, 80
Maloney, ShaneA., 75Mandrini, C.H., 81Mandrini, Cristina, 74Mann, R.G., 55, 61Mannering, Elizabeth, 83Manoharan, P.K., 75Mao, Shude, 83Marconi, Marcella, 62Marcu, A., 61Marengo, M., 78Maria, Anna, 69Marin, Felipe, 77Markwick, Andrew, 65Marquette, Jean-Baptiste, 62Marsden, Richard, 54Marsh, M., 48, 54, 85Marsh, Mike, 60Marsh, T.R,77Martin, S., 64Martin-Pintado, J., 64Martinez-Oliveros, J.C., 60Mason, Andrew, 46Mason, H., 80Mason, H.E., 85Mason, Helen, 49, 86, 88Massi, F., 72Masson, A., 47Massone, and, 69Massone, AnnaMaria, 56Masters, Adam, 52Mathioudakis, M., 87Mathioudakis, Mihalis, 60Matsuura, M., 51, 78Matsuura, Mikako, 58Matthews, Brenda, 51Matthews, S.A., 69Matthews, Sarah, 48, 74Matthews, SarahA., 74Mauch, Thomas, 44Mauskopf, Phil, 89Mawson, Neil, 49Maxted, P.F.L., 78Mayer, L., 57McCaughrean, Mark, 42McCaughrean, MarkJ., 51McClements, K.G., 88McConnachie, A., 57McConville, S.L., 59, 70McCord, K., 73McCoustra, Martin, 63, 65McCoustra, MartinR.S., 64McCracken, T., 73McCrea, I., 67McDermott, A., 47McDonald, I., 78McHardy, Ian, 63McKean, John, 50McKinnell, L.-A., 67McLaughlin, James, 88McLay, Sam, 65McMahon, Richard, 62McQuillin, Rachael, 83McWhirter, I., 67Meixner, M., 78Melrose, Don, 43MESS consortium, 51Messineo, M., 46Meyer, Karen, 80Michaud, Peter, 86Middleton, H.R., 67Miki, Z., 75Milan, S.E., 47, 53, 66, 67, 76Milan, Steve, 74Millar, Tom, 65Miller, David, 72Miller, Grant, 85Miller, Steve, 59Minnitti, D,62
Mitchell, Cathryn, 67MitraKraev, Urmila, 80MMB Collaboration, 45Monnier, John, 72, 73Moretti, MariaIda, 62Morgan, H., 75Moro-Martin, Amaya, 51Mortlock, Daniel, 76Morton, Richard, 60, 86Mouikis, C., 47Murphy, David, 77MUSYC Collaboration, 78Muxlow, T,50Muxlow, T.W.B., 50Muxlow, Tom, 63, 71Myers, AdamD., 77Ménard, F., 72
Nakariakov, V.M., 60, 88Nandra, Kirpal, 82, 84Natta, A., 72Negueruela, I., 46Nelson, Richard, 43Neukirch, Thomas, 59, 69, 74New, R., 86NGLS teammembers, 45Ngwira, C.M., 67Nicerkson, Sarah, 84Nichol, R., 50, 77Nichol, Robert, 77Nichols, Jonathan, 52Nielbock, M., 64Nishino, M.N., 47Norton, A.J., 46Nutter, David, 49Nykyri, K., 47
O'Brien, P.T., 71O'Dwyer, Brendan, 88O'Neil, Robert, 49Oieroset, M,47Olivares, A., 73Ollivier, M., 90Opher, M., 85Opperman, B., 67Orza, Beniamin, 61Oudmaijer, R.D., 46Oudmaijer, Rene, 72Owen, C.J., 47, 48, 69, 75Owen, Christopher, 54Owens, M.J., 75Owens, Mathew, 75Owens, Steve, 87
PACS consortium, 50Parnell, Clare, 74Parsons, H., 46Pascoe, David, 61Pastorello, A., 70Patel, Harsit, 50Patel, Prina, 50Patience, J., 63, 84Patience, Jenny, 51, 73Peacock, John, 57, 63Pearson, J., 54Pedlar, Alan, 71Pedram, Ehsan, 74Pedretti, E., 73Pedretti, Ettore, 73Penarrubia, Jorge, 57Penny, Alan, 50Percival, Susan, 79Percival, WillJ,77Perlman, E.S., 83Perrett, K., 57Perrin, G., 73Perry, Chris, 75Persoon, A.M., 66
94
Pestaña, JoséLuisGarrido, 71Petit, Pascal, 73Petkaki, Panagiota, 68Petrosian, V., 63Phan, T.D., 47Phelps, A.D.R., 59, 70Phillipps, S., 55, 77Phillips, Neil, 51Piana, Michele, 56, 69Pilkington, Kate, 84Pinfield, David, 77Pintér, B., 75Pitkin, Matthew, 82, 82Plez, B., 73Poglitsch, A., 64Polehampton, E., 51Polehampton, E.T., 58Pollacco, D., 42, 55Pontin, David, 74, 74Pontin, DavidI., 74Pope, A., 44Popescu, CristinaC., 45Popescu, M., 85Potts, Hugh, 80Potts, HughE., 80Power, C., 63Predoi, Valeriu, 71Prescott, Matthew, 45Price, J., 77Priest, E.R., 74Prinja, Raman, 45Pritchet, C., 57Provan, G., 65Provan, Gabby, 67Pryse, S.E., 59, 67Pu, Z., 47
Rae, I.J., 47Raeder, Joachim, 74Rahimi, Awat, 45Rangel, Cyprian, 84Ratcliffe, Heather, 69Rawlings, Steve, 50, 63, 83Rea, Alex, 73Reach, W.T., 78Read, Justin, 57Read, M., 61Read, M.A., 55Read, Mike, 54, 55, 62Reay, Sarah, 65Redfield, S., 58Reid, H.A.S., 69Reid, Hamish, 69Rekjuba, M,62Relano, Monica, 78Rhodes, R., 73Rice, Ken, 55Richards, Anita, 58, 73Richer, J.S., 46Richer, John, 50Rigby, Emma, 51, 63Rigopoulou, Dimitra, 45, 50Riley, P., 75Ripepi, Vincenzo, 62RMS Team, 46Roberts, Helen, 65Robertson, C.W., 59Robertson, David, 61Robinson, Terry, 67Robinsson, David, 89Robotham, Aaron, 44, 45Roche, P., 46Rodger, Craig, 65Ronald, K., 70Ronald, Kevin, 59Rosa, RobertDe, 51Ross, Ashley, 77Ross, Nicholas, 77
Roth, M., 86Rottgering, Huub, 63Rouillard, Alexis, 75Rowlinson, Antonia, 71Roxburgh, I., 86Ruderman, M.S., 61Ruffle, Paul, 65Rushton, M.T., 46Rushton, Mark, 46Ryans, R.S.I., 87Rycroft, Michael, 66
Sabiu, Cristiano, 77SAGE-Specteam, 79Saha, Prasenjit, 78Sahraoui, F., 47Saito, R,62Sakai, Satoru, 82Salucci, Paolo, 72Sanchez-Blazquez, P., 83Sanderson, A., 56Santoro, F., 73Sargent, A., 63Sargent, B.A., 78Sathyaprakash, Bangalore, 43Saunders, Richard, 63Sauvage, M., 64Schawinski, Kevin, 78Schinnerer, E., 64Schmieder, B., 88Schneider, M., 63Schreiber, J., 64Schwadron, Nathan, 75SDSS-II SNeSurveyTeam, 77SDSS-III:BOSS Team, 77Semionov, Dmitrij, 45Senior, A., 68Senior, Andrew, 67Sergis, N., 66Sharples, Ray, 50ShaunBloomfield, D., 88Shay, M.A., 47Sheldon, ErinS., 77Shelyag, S., 61Shelyag, Sergiy, 60Shen, C., 47Shetty, Vineeth, 75Shi, J., 47Shishov, V.I., 75Shtromberg, A., 73Sibbons, Lisette, 79Sibeck, David, 74Sibthorpe, Bruce, 51Silk, Joe, 56Silk, Joseph, 78Simpson, Fergus, 57Singal, S., 63Sivasankaran, Anoop, 56Sivia, Devinder, 83Sloan, G.C., 78Slyz, Adrianne, 83Smail, Ian, 44, 63Smartt, S., 70Smecker-Hane, T., 78Smith, Anthony, 51Smith, Arfon, 55Smith, G.P., 56Smith, James, 55Smith, Mathew, 77Smith, Matthew, 51Smith, Rachel, 73Smith, Russell, 79Sobral, David, 44Sochting, I.K., 83Southwood, David, 52Spain, Timothy, 67, 79Speck, A.K., 78Speirits, Fiona, 57
Speirs, D.C., 59Speirs, David, 70Spencer, P,67SPIRE consortium, 50Stallard, Tom, 59Stamatellos, D., 51Stanway, Elizabeth, 78Stappers, B., 82Stark, C.R., 81Stark, C.R., 82Stark, Craig, 70Stavrinidis, Constantinos, 89Stawarsz, L., 63Steed, Kimberley, 75Steeghs, D., 77Steele, I.A., 49Steele, Iain, 49Sternberg, A., 64Stevens, Jason, 83Steves, Bonnie, 56Stinson, Greg, 84, 84Stott, J., 43Strachan, Mel, 90Sturm, E., 64Subramanian, Srividya, 76, 81Sullivan, M., 57Sullivan, Mark, 71Sun, Jian, 54sunearthplan.netteam, 87Suntrekteam, 86Sutherland, Will, 62, 62Sutorius, E., 61Sutorius, Eckhard, 54, 62Swain, M., 90Sweatman, Winston, 56SwiftTeam, 70Swinyard, B., 52Swinyard, BruceM., 58
Tacconi, L., 64Takato, Naruhisa, 44Takats, K., 70Tamura, Naoyuki, 44Tan, BoonKok, 45Tang, Y.H., 69Tanvir, N., 78Tanvir, N.R., 71Tanvir, Nial, 43Targett, T., 56Taroyan, Y., 61Tatton, Bejamin, 79Tatulli, E., 72Taylor, Andy, 72Taylor, M.G.G.T., 47Taylor, Matt, 47Teodoro, L.F.A., 57, 81, 82Teodoro, LuisF.A., 57, 58Tessenyi, M., 90Th. vanLoon, J., 78Thatte, Niranjan, 89THESIS team, 90Thompson, M., 46, 86Thompson, M.J., 61Thomson, A.W.P., 67, 79Thomson, Alan, 66Thomson, AlanP,65Thomson, andAlan, 65Thomson, Edward, 57Threlfall, James, 88Tideswell, David, 65Tielens, A.G.G.M., 78Tinetti, G., 58Tinetti, Giovanna, 90Tokumaru, M., 75Tout, Christopher, 78Tripathi, Durgesh, 49Trotta, Roberto, 76Trung, Dinhvan, 73
95
Tsiklauri, David, 81Tuffs, RichardJ., 45Tunnicliffe, Rachel, 71Turkmani, Rim, 70Turnbull, Katie, 79Turner, A., 47Tyul’bashev, S.A., 75
UltraVISTA consortium, 62Usuda, KumikoS., 86
vanBallegooijen, A.A., 76, 80VanDoorsselaere, Tom, 61vanDriel-Gesztelyi, Lidia, 76, 81vanSpaandonk, Lieke, 77Vanninathan, Kamalam, 81VargasDominguez, Santiago, 49Vasisht, G., 90Vekstein, G.E., 68Verma, A., 64Verth, G., 60Verth, Gary, 61Verwichte, E., 88VHS collaboration, 62Vickers, Hannah, 67VIDEO Consortium, 62Vidotto, Aline, 85Vigroux, L., 64VIKING Team, 62VirgoCollaboration, 71Viti, S., 64Viti, Serena, 64Vlahos, Loukas, 70VMC Team, 61, 62Volwerk, M., 47Vorgul, I., 59, 70
Wadsley, James, 84Waldmann, Ingo, 58Walker, Helen, 87Walker, M., 57Walker, Matthew, 57Wall, Jasper, 63Wallace, Alison, 74, 87Walsh, A.P., 47, 75
Walsh, Andrew, 48Walsh, R.W., 48, 60, 85Walsh, Robert, 54Walter, F., 64Walter, F.M., 84Wang, Yougang, 84Ward, Martin, 71Ward-Thompson, Derek, 51Wardle, Nick, 61WASP Consortium, 42WASP Consortium, 55Watanabe, T., 48Waterson, Natasha, 75Watson, Fraser, 89Watson, Laura, 76Watt, C., 47Weltevrede, P., 82Weltevrede, Patrick, 59Wesson, Roger, 51, 58West, R., 42West, R.G., 55Westmoquette, Mark, 84Whaler, Kathy, 43Wheatley, Peter, 49White, G.J., 52White, Richard, 90Whitley, Toby, 66Whyte, C.G., 59Wiersema, K., 71Wilcock, L., 51Wild, J.A., 53, 59, 68, 79Wild, J.M., 85Wild, Jim, 67, 87Wilkins, G.M.H., 85Williams, Anthony, 67, 76Williams, D.A., 64Williams, David, 54Williams, DavidR., 49Williams, P., 61Williams, Peredur, 54Williger, G.M., 83Wilmot-Smith, Antonia, 74, 74Wilson, Fiona, 74Wilson, R.J., 66Wise, M., 50
Wit, W.-J.de, 46Witherick, Dugan, 58Woan, Graham, 55, 82Wood, A.G., 75Wood, Alan, 59, 67Woodcraft, A.L., 89Woodfield, Emma, 68Woods, P.M., 78Woods, Paul, 79Worrall, D.M., 83Wright, A.N., 61, 70Wright, Andrew, 70Wright, D.M., 66Wright, Gillian, 43Wu, Xufen, 84Wyatt, M.C., 73Wyatt, Mark, 51Wyper, Peter, 74Wyse, Rosie, 43
Yates, Japheth, 52Yates, Jeremy, 73Yates, JeremyA., 58Yeates, Anthony, 74, 76Yeates, AnthonyR., 74Yeche, Christophe, 77Yeoman, T.K., 53, 66Yi, Sukyoung, 78Yiu, H.-C.I., 67Young, Dave, 66Young, J., 73Young, John, 72, 73Young, Neil, 82Young, P., 48Young, Peter, 49Yu, Shenghua, 52
Zanna, GiulioDel, 49, 61, 88Zarka, P., 52Zezas, Andreas, 71Zhang, ZengHua, 77Zhao, Hongsheng, 71, 72, 84Zharkov, Sergei, 61Zijlstra, Albert, 72
96
List
of p
artic
ipan
tsAbdulgalil, Ali(Heriot-WattUniversity)
[email protected] [P17]Abernathy, Matthew(UniversityofGlasgow)
[email protected], Nicholas(UCL) [email protected]
[P13, P08]Aerts, Conny(UniversityofLeuven)
[email protected], Caroline(UCLAN)
[email protected] [P04]Ames, Susan(OxfordAstrophysics)
[email protected], David(UniversityofLeicester)
[email protected] [P18]Anthony, Caroline(ImperialCollege)
[email protected], Vasilis(UniversityofStAndrews)
[email protected] [P34]Arridge, Chris(MSSL /UCL) [email protected]
[P18, P08]Austin, Matthew(UCL) [email protected] [P02]Avison, Adam(JodrellBankCentrefor
Astrophysics) [email protected] [P02]Awad, Zainab(Dept.ofPhysicsandAstronomy,
UCL) [email protected] [P17]Badnell, Nigel(UniversityofStrathclyde)
[email protected], Gemma(UniversityofHertfordshire)
[email protected] [P15]Bagnulo, Stefano(ArmaghObservatory)
[email protected] [P32]Bailey, Mark(ArmaghObservatory) [email protected], William(RufusScientific/MIT)
[email protected] [Plenary]Baldry, Ivan(LiverpoolJMU)
[email protected] [P26]Ballai, Istvan(UniversityofSheffield)
[email protected] [P14]Barclay, Charles(MarlboroughCollegeandOxford
Astrophysics) [email protected][P33]
Bareford, Michael(TheUniversityofManchester)[email protected][P23]
Barker, Michael(RoyalObservatoryEdinburgh)[email protected] [P27]
Barnsley, Robert(LJMU) [email protected][P05]
Baron, Fabien(UniversityofMichigan)[email protected] [P22]
Barr, Ewan(MPIfR Bonn)[email protected] [P30]
Bartlett, Jo(UCL/MSSL) [email protected], Leon(UniversityofSussex)
[email protected], Riccardo(UniversityofGlasgow)
[email protected], Marina(UniversityofGlasgow)
[email protected] [P19, P34]Bayet, Estelle(UCL) [email protected] [P17, P17,
P17]Beaulieu, Jean-Philippe(UniversityCollegeof
London) [email protected], Ciaran(BritishGeologicalSurvey)
[email protected] [P18]Benisty, Myriam(INAF -Arcetri)
[email protected] [P22]Bennet, Euan(UniversityofGlasgow)
[email protected] [P13]Bentley, Robert(UCL-MSSL) [email protected]
[P24]Bento, Joao(UniversityofWarwick)
[email protected] [P05]Bergman, Jan(SwedishInstituteofSpacePhysics)
[email protected] [P35]Berry, Christopher(InstituteofAstronomy,
UniversityofCambridge) [email protected]
Best, Philip(IfA Edinburgh) [email protected] [P16,P01]
Beveridge, Nicola(UniversityofGlasgow)[email protected] [P35]
Bewsher, Danielle(UniversityofCentralLancashire) [email protected] [P09, P33]
Bian, Nicolas(UniversityofGlasgow)[email protected] [P19]
Bibby, Joanne(UniversityofSheffield)[email protected] [P02]
Birch, Martin(UniversityofCentralLancashire)[email protected]
Bird, Anthony(SAF) [email protected], Mario(AberystwythUniversity)
[email protected] [P99, P24, P34]Blake, Rob(RoyalObservatoryEdinburgh)
[email protected] [P15, P10]Bluck, Asa(UniversityofNottingham)
[email protected] [P31]Boles, Tom(CoddenhamObservatory)
[email protected], Barbara(JeremiahHorrocksInstitute,
UCLan) [email protected] [P34]Bromage, Gordon(JeremiahHorrocksInstitute,
UCLan) [email protected], Chris(UniversityofCentralLancashire)
[email protected] [P11, P31]Brooke, John(UniversityofManchester)
[email protected] [P24, P10]Brown, Daniel(UniversityofCentralLancashire)
[email protected], John(UniversityofGlasgow)
[email protected] [P19, P19]Browne, Paul(UniversityofStAndrews)
[email protected], Philippa(JBCA,Universityof
Manchester) [email protected][P19, P23]
Bruce, Victoria(IfA,UniversityofEdinburgh)[email protected]
Bryan, Sarah(UniversityofManchester)[email protected] [P31]
Buckle, Jane(UniversityofCambridge)[email protected] [P02]
Bulger, Joanna(UniversityofExeter)[email protected] [P16]
Burge, Christina(UniversityofGlasgow)[email protected] [P19]
Burke, Claire(AstrophysicsResearchInstituteLJMU) [email protected] [P01]
Buscher, David(UniversityofCambridge)[email protected] [P22, P22]
Butters, Oliver(UniversityofLeicester)[email protected] [P10]
Calura, Francesco(JeremiahHorrocksInstitute,UCLAN) [email protected] [P31]
Cameron, Andrew(UniversityofStAndrews)[email protected] [Plenary]
Campsie, Paul(UniversityofGlasgow)[email protected]
Cano, Zach(ARI,JohnMooresUniversityLiverpool) [email protected] [P20]
Cargill, Peter(ImperialCollege)[email protected] [P29]
Carozzi, Tobia(Univ.ofGlasgow)[email protected] [P10]
Carpineti, Alfredo(ImperialCollege)[email protected] [P01]
Carr, Chris(ImperialCollegeLondon)[email protected] [P09]
Chaplin, William(UniversityofBirmingham)[email protected]
Chapman, Bob(UniversityofIceland)[email protected]
Chapman, Sean(UniversityofManchester)[email protected] [P17]
Chapman, Steven(UniversityofCentralLancashire) [email protected] [P34]
97
Charnley, Steven(NASA GoddardSpaceFlightCenter) [email protected] [P17]
Chorley, Nicky(UniversityofWarwick)[email protected] [P14]
Christie, Helen(UniversityCollegeLondon)[email protected] [P17]
Christodoulou, Leonidas(UniversityofSussex)[email protected] [P01]
Christopher, Natalie(UniversityofOxford)[email protected] [P17]
Chrysostomou, Antonio(JointAstronomyCentre)[email protected]
Cioni, Maria-Rosa(UniversityofHertfordshire)[email protected] [P27, P27, P15, P15,P15]
Clark, Simon(OpenUniversity)[email protected] [P02]
Clarke, Ellen(BritishGeologicalSurvey)[email protected] [P18]
Clarke, Fraser(UniversityofOxford)[email protected] [P35]
Clements, David(None) [email protected][P05]
Clowes, Roger(Univ.ofCentralLancashire)[email protected]
Clube, Kim(RoyalAstronomicalSociety)[email protected]
Collings, Mark(Heriot-WattUniversity)[email protected]
Collins, Ross(IfA,Edinburgh) [email protected] [P15,P15, P10]
Cooper, Heather(UniversityofLeeds)[email protected] [P02]
Cossham, Jennifer(JohnWiley&Sons, Ltd)[email protected]
Crockett, Philip(Queen'sUniverstyBelfast)[email protected] [P14, P14]
Cross, Nicholas(IfA,Edinburgh) [email protected][P15]
Crowther, Paul(UniversityofSheffield)[email protected] [P02, P27]
Culhane, Len(MSSL/UCL) [email protected][P04, P09]
Cunningham, Colin(UK AstronomyTechnologyCentre) [email protected][Plenary]
CurtisLake, Emma(UniversityofOxford)[email protected] [P01]
Dalla, Silvia(UniversityofCentralLancashire)[email protected] [P19]
Davidson, Michael(IfA,Edinburgh) [email protected], Ben(RochesterInstituteofTechnology,
NY) [email protected] [P02]Davies, Jackie(RutherfordAppletonLaboratory)
[email protected], Roger(UniversityofOxford)
[email protected], Christopher(STFC RutherfordAppleton
Laboratory) [email protected] [P24]Davis, Gary(JointAstronomyCentre)
[email protected] [P05]Davis, Olaf(Oxford) [email protected]
[P11]Dawson, Ewan(BritishGeologicalSurvey)
[email protected] [P18]DeRosa, Robert(UniversityofExeter)
[email protected] [P32]DePasquale, Massimiliano(UCL/MSSL)
[email protected] [P20]Deane, Roger(Oxford)
[email protected] [P16]DelZanna, Giulio(UniversityofCambridge)
[email protected] [P04]Dere, Ken(GeorgeMasonUniversity)
[email protected] [P34]Dickson, Ewan(UniversityofGlasgow)
[email protected] [P19]Ding, Jiaoyang(ArmaghObservatory)
[email protected] [P29]Diver, Declan(UniversityofGlasgow)
[email protected] [P30, P29]Dominik, Martin(SUPA,UniversityofStAndrews)
[email protected], Emile(UniversityofSheffield)
[email protected], Gareth(Queen'sUniversityofBelfast)
[email protected] [P34]Dougherty, Michele(ImperialCollegeLondon)
[email protected] [P09]Down, Emily(UK GeminiSupportGroup)
[email protected] [P31]Doyle, Gerry(ArmaghObservatory)
[email protected] [P08]Doyle, Simon(CardiffUNiversity)
[email protected] [P35]Drake, Alyssa(LJMU) [email protected], James(UniversityofEdinburgh)
[email protected] [P15]Duthie, Roger(MSSL,UCL) [email protected]
[P03]Eastwood, Jonathan(ImperialCollegeLondon)
[email protected] [P03]Efstathiou, George(KavliInstituteforCosmology)
[email protected] [Plenary]Eldridge, John(InstituteofAstronomy(Cambridge))
[email protected] [P27]Elliott, David(RoyalAstronomicalSociety)
[email protected], Jim(QueenMary, UnivofLondon)
[email protected] [P15]Enoch, Becky(UniversityofStAndrews)
[email protected], Barbara(UniversityofExeter)
[email protected], C. Philippe(ESA/ESTEC)
[email protected] [P03]Espinoza, Cristobal(JodrellBankCentrefor
Astrophysics) [email protected] [P30]Evans, Christopher(UK ATC) [email protected] [P02,
P27]Eyres, Stewart(UniversityofCentralLancashire)
[email protected], James(UniversityofHertfordshire)
[email protected] [P31]Fanidakis, Nikolaos(DurhamUniversity)
[email protected], Jay(UniversityofLeicester)
[email protected] [P12]Fazakerley, Andrew(MSSL-UCL)
[email protected] [P03]Fear, Robert(UniversityofLeicester)
[email protected] [P23]Feix, Martin(UniversityofStAndrews)
[email protected] [P31, P21, P21]Ferdman, Robert(UniversityofManchester)
[email protected] [P30]Ferreras, Ignacio(MSSL/UCL)
[email protected] [P27, P01, P11]Findlay, Joseph(QMUL) [email protected]
[P15]Fletcher, Lyndsay(UniversityofGlasgow)
[email protected] [P34, P29, P19,P04, P19, P29]
Fleuren, Simone(QueenMaryUniversityLondon)[email protected]
Fludra, Andrzej(STFC RutherfordAppletonLaboratory) [email protected] [P09,P09]
Forgan, Duncan(SUPA,IfA,UniversityofEdinburgh) [email protected] [P10]
Forsyth, Colin(UCL MSSL) [email protected][P03]
Frankland, Victoria(Heriot-WattUniversity)[email protected] [P17]
Fraser, HelenJane(SUPA,UniversityofStrathclyde) [email protected]
Fraser, Morgan(QueensUniversityBelfast)[email protected] [P20]
Frenk, Carlos(DurhamUniversity)[email protected] [P11]
Fullekrug, Martin(UniversityofBath)[email protected] [P18]
Fuller, Gary(JodrellBankCentreforAstrophysics-UK ALMA ARC)[email protected] [P17, P02, P17,P17]
Gaensicke, Boris(UniversityofWarwick)[email protected] [P26]
Gallagher, Peter(TrinityCollegeDublin)[email protected] [P24]
Garcia, Percival(Percival&Associates)[email protected]
Garrett, Michael(ASTRON) [email protected], Simon(UniversityofManchester)
[email protected] [P05, P20]Gascoyne, Andrew(UniversityofSheffield)
[email protected], Sam(OxfordAstrophysics)
[email protected] [P31]Ghodsi, Hoda(UniversityofGlasgow)
[email protected] [P11]Gibson, Brad(UnivofCentralLancashire)
[email protected] [P31]Gibson, Heather(OpenUniversity)
[email protected], Colin(UniversityofGlasgow)
[email protected], Gerard(InstituteofAstronomy)
[email protected], Pedro-Alejandro(Sheffield
University) [email protected], Marcel(K.U.Leuven-CPA)
[email protected], James(UniversityofCambridge)
[email protected] [P22]Gordovskyy, Mykola(UniversityofManchester)
[email protected] [P19]Gosling, Andrew(Gemini, Oxford)
[email protected], Keith(UniversityofStAndrews)
[email protected] [P19, P19]Grady, Monica(TheOpenUniversity)
[email protected], David(GlasgowUniversity)
[email protected] [P04]Granot, Jonathan(UniversityofHertfordshire)
[email protected] [P20]Gray, Norman(UniversityofGlasgow)
[email protected] [P10]Green, Lucie(UCL-MSSL) [email protected]
[P09, P33, P04]Gregory, Scott(UniversityofExeter)
[email protected] [P32]Griffin, Matt(CardiffUniversity)
[email protected] [P07]Grocott, Adrian(UniversityofLeicester)
[email protected] [P18]Guandalini, Roald(UniversityofHertfordshire)
[email protected] [P15]Guo, Jingnan(UniversityofGlasgow)
[email protected] [P19]Gupta, Jennifer(JodrellBankCentrefor
Astrophysics)[email protected][P01]
Gürkan, Gülay(TheUniverstiyofManchester)[email protected][P21]
Habergham, Stacey(AstrophysicsResearchInstitute) [email protected] [P02]
Hallinan, Gregg(UC Berkeley)[email protected] [P08]
Hambly, Nigel(UniversityofEdinburgh)[email protected] [P10, P15, P10]
98
Hamilton-Morris, Victoria(UniversityofBirmingham) [email protected] [P11]
Hannah, Iain(UniversityofGlasgow)[email protected] [P19, P19, P34, P04]
Hapgood, Mike(STFC RutherfordAppletonLaboratory) [email protected] [P24,P09, P03]
Hargreaves, John(UniversityofLancaster)[email protected] [P28]
Harra, Louise(UCL-MSSL) [email protected][P09, P09]
Harris, Jennifer(UniversityofWarwick)[email protected] [P34]
Harris, Kathryn(UCLan) [email protected][P31]
Harrison, Richard(RutherfordAppletonLaboratory) [email protected][P09]
Hatchell, Jennifer(UniversityofExeter)[email protected] [Plenary]
Haughian, Karen(UniversityofGlasgow)[email protected]
Hawken, Adam(UCL) [email protected], Alan(UniversityofEdinburgh)
[email protected] [P21, P21]Hebden, Kerry(JodrellBankCenterfor
Astrophysics)[email protected][P17]
Henault-Brunet, Vincent(InstituteforAstronomy,UniversityofEdinburgh) [email protected]
Hendry, Martin(UniversityofGlasgow)[email protected] [P11, P33, P33]
Heng, IkSiong(UniversityofGlasgow)[email protected] [P30]
Hepburn, Ian(UCL/MSSL) [email protected][P35]
Hermanowicz, Maciej(InstituteofAstronomy,UniversityofCambridge) [email protected]
Heward, Anita(RoyalAstronomicalSociety)[email protected]
Heyer, Inge(JointAstronomyCentre)[email protected] [P33]
Heymans, Catherine(IfA,UniversityofEdinburgh)[email protected] [P21]
Higgins, Paul(TrinityCollegeDublin)[email protected] [P34]
Hild, Stefan(UniversityofGlasgow)[email protected] [P35]
Hill, David(UniversityofStAndrews)[email protected] [P01, P01]
Hillier, Dan(RoyalObservatoryEdinburghVisitorCentre) [email protected] [P33]
Ho, Wynn(UniversityofSouthampton)[email protected] [P30]
Holland, Wayne(UK AstronomyTechnologyCentre) [email protected]
Holliman, Mark(UniversityofEdinburgh, InstituteforAstronomy) [email protected] [P10,P10]
Hood, Alan(UniversityofStAndrews)[email protected] [P04]
Hood, Ross(InstituteforAstronomy, UniversityofEdinburgh) [email protected]
Horn, Markus(ImperialCollegeLondon)[email protected] [P11]
Horne, Keith(SUPA StAndrews)[email protected]
Hornig, Gunnar(UniversityofDundee)[email protected] [P23, P23]
Hough, James(UniversityofHertfordshire)[email protected]
House, Elisa(UniversityofCentralLancashire)[email protected] [P31]
Hsieh, Henry(QueensUniversityBelfast)[email protected] [P12]
Huang, Zhenghua(ArmaghObservatory)[email protected] [P29]
Hudson, Hugh(SSL/UC Berkeley)[email protected] [P29, P14]
Husnoo, Nawal(UniversityofExeter)[email protected]
Hussain, Gaitee(ESO) [email protected] [P32]Hutcheon, Richard(KeeleUniversity)
[email protected] [P27]Hutchinson, James(UniversityofLeicester)
[email protected] [P18]Huxor, Avon(UniversityofBristol)
[email protected] [P26, P10]Hyde, Paul(None) [email protected], Edo(UK AstronomyTechnologyCentre)
[email protected] [P01]Jain, Rekha(UniversityofSheffield)
[email protected] [P23]Jarvis, Matt(UniversityofHertfordshire)
[email protected] [P31, P15, P06]Jeffries, Rob(KeeleUniversity)
[email protected] [P32]Jess, David(Queen'sUniversityBelfast)
[email protected] [P14, P14, P14]John, Daniel(DurhamUniversity)
[email protected] [P11]Johnson, Olivia(RoyalObservatoryGreenwich)
[email protected] [P33]Johnston, Rebecca(UniversityofCambridge)
[email protected], Russell(UniversityoftheWesternCape)
[email protected] [P01]Johnstone, Colin(UniversityofStAndrews)
[email protected], Geraint(MSSL,UCL) [email protected]
[P18, P13]Jones, Mark(TheOpenUniversity)
[email protected] [P10]Jones, Olivia(UniversityofManchester)
[email protected][P27]
Jonsson, Jakob(UniversityofOxford)[email protected] [P11]
Jordan, Carole(UniversityofOxford)[email protected]
Kanani, Sheila(MullardSpaceScienceLaboratory)[email protected] [P18]
Karczewski, Oskar(UCL)[email protected]
Kaviraj, Sugata(ImperialCollegeLondon)[email protected] [P27]
Kellett, Stephanie(UniversityofLeicester)[email protected] [P18]
Kelly, Gemma(UniversityofLiverpool)[email protected] [P18]
Kelly, James(UCLan) [email protected], Lee(StAndrews) [email protected]
[P01, P01]Kennedy, Julia(InstituteforAstronomy, University
ofEdinburgh) [email protected] [P35]Keogh, Dominic(DurhamUniversity)
[email protected] [P30]Kerr, John(None) [email protected], Peter(Queen'sUniversityBelfast)
[email protected], Robert(LancasterUniversity)
[email protected] [P13]Kiessling, Alina(UniversityofEdinburgh)
[email protected] [P21]Kim, Hansik(DurhamUniversity)
[email protected] [P16]King, Robert(UniversityofExeter)
[email protected] [P08]Kipping, David(Harvard-SmithsonianCenterfor
Astrophysics) [email protected] [P12]Kitching, Thomas(UniversityofEdinburgh)
[email protected], Khurom(UniversityofWarwick)
[email protected] [P03]Kofman, Wlodek(LPG CNRS/UJF)
[email protected], Eduard(UniversityofGlasgow)
[email protected] [P19, P19, P19, P34,P19, P19, P19, P19]
Kukula, Marek(RoyalObservatoryGreenwich)[email protected] [P24, P33]
Kunawicz, Nadya(JodrellBankCentreforAstrophysics) [email protected][P17]
Kurtz, Donald(UniversityofCentralLancashire)[email protected] [P33]
Kuznetsov, Alexey(ArmaghObservatory)[email protected] [P08]
Labrosse, Nicolas(UniversityofGlasgow)[email protected] [P34]
Lacerda, Pedro(Queen'sUniversityBelfast)[email protected] [P12]
Lacey, Cedric(DurhamUniversity)[email protected] [P07]
Lang, Pauline(UniversityofStAndrews)[email protected] [P08]
Lawrence, Andy(UniversityofEdinburgh)[email protected] [P16]
Lawrie, Craig(UniversityofGlasgow)[email protected] [P11]
Lester, Mark(UniversityofLeicester)[email protected] [P09, P18]
Levan, Andrew(UniversityofWarwick)[email protected] [P30]
Lewis, Fraser(FaulkesTelescopeProject)[email protected]
Lewis, James(InstituteofAstronomy)[email protected] [P15]
Li, Chuan(MullardSpaceScienceLaboratroy)[email protected] [P19]
Li, Xing(AberystwythUniversity) [email protected][P34]
Liang, Guiyun(UniversityofStrathclyde)[email protected] [P29]
Liddle, Andrew(UniversityofSussex)[email protected]
Lin, Bob(Univ.ofCalifornia, Berkeley)[email protected] [Plenary]
Lintott, Chris(UniversityofOxford)[email protected] [P24, P10]
Littlefair, Stuart(UniversityofSheffield)[email protected] [P08]
Liu, Siming(UniversityofGlasgow)[email protected] [P19, P19]
Loveday, Jon(UniversityofSussex)[email protected] [P01, P26]
Lowe, Stuart(TheJodcast)[email protected] [P33]
Lowes, Frank(NewcastleUniversity)[email protected]
Lucas, Philip(UniversityofHertfordshire)[email protected] [P15]
Lucek, Elizabeth(ImperialCollege)[email protected] [P03, P09, P09]
Lumsden, Stuart(UniversityofLeeds)[email protected]
Luna, Marialejandra(UniversityofSheffield)[email protected] [P14]
Lykou, Foteini(Claire)(JodrellBankCentreforAstrophysics)[email protected][P22]
MacKinnon, Alec(UniversityofGlasgow)[email protected] [P19, P19, P33]
MacTaggart, David(StAndrews)[email protected] [P34]
Macdonald, Erin(UniversityofGlasgow)[email protected] [P01]
Mackay, Craig(InstituteofAstronomy, UniversityofCambridge) [email protected]
Mackay, Duncan(UniversityofStAndrews)[email protected]
Mackay, Mel(InstituteofAstronomy, Universityof
99
Cambridge) [email protected], Maria(ArmaghObservatory)
[email protected] [P29, P29]Majewski, Pawel(RutherfordAppletonLaboratory)
[email protected] [P11, P11]Mallik, Procheta(UniversityofGlasgow)
[email protected] [P29]Mannering, Elizabeth(UniversityofBristol)
[email protected] [P31]Marsden, Richard(ESA) [email protected]
[P09]Marsh, Mike(UniversityofCentralLancashire)
[email protected] [P14]Mason, Andrew(OpenUniversity)
[email protected] [P02]Mason, Helen(UniversityofCambridge)
[email protected] [P33, P04, P34]Massey, Robert(RoyalAstronomicalSociety)
[email protected], AnnaMaria(CNR-SPIN)
[email protected] [P10]Masters, Adam(MullardSpaceScience
Laboratory) [email protected] [P08]Masters, Richard(OxfordUniversity)
[email protected], Mihalis(QueensUniversityBelfast)
[email protected] [P14, P14]Matsuura, Mikako(UniversityCollegeLondon)
[email protected] [P12]Matthews, Sarah(UCL-MSSL) [email protected]
[P04, P23]Mawson, Neil(AstrophysicsResearchInstitute)
[email protected] [P05]Maxted, Pierre(KeeleUniversity)
[email protected], Michael(UCLan)
[email protected], Mark(ESA) [email protected] [Plenary]McCombie, June(UniversityofNottingham)
[email protected], Martin(Heriot-WattUniversity)
[email protected] [P17, P17]McKean, John(ASTRON) [email protected] [P06]McLauchlan, Rachael(UniversityofGlasgow)
[email protected], James(NorthumbriaUniversity)
[email protected][P34]
McMahon, Richard(UniversityofCambridge)[email protected] [P15]
McQuillin, Rachael(KeeleUniversity)[email protected] [P31]
Mecheri, Redouane(QueenMaryUniversityofLondon) [email protected]
Melrose, Don(UniversityofSydney)[email protected] [Plenary]
Meyer, Karen(UniversityofStAndrews)[email protected] [P29]
Meyerdierks, Horst(RoyalObservatoryEdinburgh)[email protected]
Miller, David(UniversityofGlasgow)[email protected] [P21]
Miller, Grant(UniversityofStAndrews)[email protected] [P32]
Miller, Steve(UCL) [email protected] [P13]Mitchell, Cathryn(UniversityofBath)
[email protected] [P18]MitraKraev, Urmila(UniversityofCambridge
(DAMTP)) [email protected][P29]
Moretti, MariaIda(BolognaUniversity)[email protected] [P15]
Morgan, Lawrence(LiverpoolJohnMooresUniversity) [email protected]
Morris, Margaret(AstronomicalSocietyofGlasgow) [email protected]
Morton, Richard(UniversityofSheffield)[email protected] [P14, P33]
Murphy, David(DurhamUniversity)[email protected] [P26]
Murray, Peter(SUPA InstututeforGravitationalResearch) [email protected]
Muxlow, Tom(JodrellBankCentreforAstrophysics) [email protected] [P20, P16]
Nelson, Richard(QueenMary, UniversityofLondon) [email protected] [Plenary]
Neukirch, Thomas(UniversityofSt.Andrews)[email protected] [P19, P23, P13]
Nicholls, Bella(RoyalAstronomicalSociety)[email protected]
Nichols, Jonathan(UniversityofLeicester)[email protected] [P08]
Norberg, Peder(IfA,UniversityofEdinburgh)[email protected]
Norton, Andrew(TheOpenUniversity)[email protected]
Nutter, David(CardiffUniversity)[email protected] [P05]
O'Brien, Paul(UniversityofLeicester)[email protected]
O'Connor, Terry(STFC) [email protected]'Dwyer, Brendan(UniversityofCambridge)
[email protected] [P34]O'Neil, Robert(UCL MSSL) [email protected]
[P04]O'Regan, Jonathan(MSSL/UCL)
[email protected], Beniamin(TheUniversityofSheffield)
[email protected] [P14]Oudmaijer, Rene(UniversityofLeeds)
[email protected] [P22]Owen, Christopher(UCL/MSSL)
[email protected] [P09]Owens, Mathew(UniversityofReading)
[email protected] [P24]Owens, Steve(IYA2009)
[email protected] [P33]Parkinson, Hannah(IfA,Edinburgh) [email protected]
[P01]Parley, Neil(UniversityofStAndrews)
[email protected], Clare(UniversityofStAndrews)
[email protected] [P23]Pascoe, David(UniversityofStAndrews)
[email protected] [P14]Pastrav, BogdanAdrian(UCLan)
[email protected], Harsit(ImperialCollegeLondon)
[email protected] [P07]Patel, Prina(InstitueofCosmology&Gravitation)
[email protected] [P06]Patience, Jenny(UniversityofExeter)
[email protected] [P22, P08]Patterson, Brett(UniversityofCentralLancashire)
[email protected], Elizabeth(CardiffUniversity)
[email protected], Ehsan(UCL MSSL) [email protected]
[P23]Pedretti, Ettore(SUPA,UniversityofStAndrews)
[email protected] [P22]Penarrubia, Jorge(UniversityofCambridge, IoA)
[email protected] [P11]Penny, Alan(U StAndrews)
[email protected] [P06]Percival, Susan(LiverpoolJohnMooresUniversity)
[email protected] [P27]Phillips, Neil(InstituteforAstronomy, University
ofEdinburgh) [email protected] [P07]Piana, Michele(Universita'diGenova)
[email protected] [P10, P19]Pilkington, Kate(UnivofCentralLancashire)
[email protected] [P31]Pitkin, Matthew(UniversityofGlasgow)
[email protected] [P30, P99, P30]Pollacco, Don(QueensUniversityBelfast)
[email protected], Frederic(UniversityofExeter)
[email protected], David(UniversityofDundee)
[email protected] [P23, P23]Popescu, CristinaC. (UCLan)
[email protected] [P01]Potts, Dale(MullardSpaceScienceLaboratory,
UCL) [email protected], Hugh(UniversityofGlasgow)
[email protected] [P29]Predoi, Valeriu(CardiffUniversity)
[email protected] [P20]Prescott, Matthew(LJMU AstrophysicsResearch
Institute) [email protected] [P01]Provan, Gabby(UniversityofLeicester)
[email protected] [P18]Quinn, Ciara(CardiffUniversity)
[email protected], Awat(MSSL (UCL)) [email protected]
[P01]Rainnie, John(RAL) [email protected], Gavin(ArmaghObservatory)
[email protected], Cyprian(ImperialCollegeLondon)
[email protected] [P31]Ratcliffe, Heather(UniversityofGlasgow)
[email protected] [P19]Rawlings, Steve(UniversityofOxford)
[email protected] [P16, P31, P06]Rea, Alex(UniversityofCambridge)
[email protected] [P22]Read, Justin(UniversityofLeicester)
[email protected] [P11]Read, Mike(IfA,UniversityofEdinburgh)
[email protected] [P10, P15, P10]Reay, Sarah(BritishGeologicalSurvey)
[email protected] [P18]Regnart, Horace(None) [email protected], Hamish(UniversityofGlasgow)
[email protected] [P19]Richards, Anita(JBCA,UniversityofManchester)
[email protected] [P22, P12]Richer, John(Cambridge) [email protected] [P05]Rigby, Emma(UniversityofNottingham)
[email protected] [P07, P16]Rigopoulou, Dimitra(STFC RAL/Oxford)
[email protected] [P01, P05]Roberts, Bernard(StAndrews)
[email protected], David(SheffieldUniversity)
[email protected] [P14]Robotham, Aaron(StAndrews)
[email protected] [P01, P01, P01]Robson, Ian(UKATC) [email protected], Paul(FaulkesTelescopeProject/Cardiff
University)[email protected]
Ronald, Kevin(UniversityofStrathclyde)[email protected] [P13]
Ross, Ashley(UniversityofPortsmouth)[email protected] [P26]
Ross, Nicholas(LawrenceBerkeleyLab)[email protected] [P26]
Rowlinson, Antonia(UniversityofLeicester)[email protected] [P20]
Ruffle, Paul(JodrellBankCentreforAstrophysics)[email protected] [P17]
Rushton, Mark(UniversityofCentralLancashire)[email protected] [P02]
Sabiu, Cristiano(None) [email protected] [P26]Sakai, Satoru(UniversityofGlasgow)
[email protected] [P30]Salaris, Maurizio(ARI -LiverpoolJohnMoores
University) [email protected], Ignacio(UniversityofGlasgow)
[email protected], Bangalore(CardiffUniversity)
100
[email protected] [Plenary]Selway, Kirsty(UniversityofGlasgow)
[email protected], Dmitrij(UCLan)
[email protected] [P01]Senior, Andrew(LancasterUniversity)
[email protected] [P18]Sharples, Ray(UNIVERSITY OF DURHAM)
[email protected] [P05]Sibbons, Lisette(UniversityofHertfordshire)
[email protected] [P27]Sibthorpe, Bruce(UK ATC)
[email protected] [P07]Simpson, Chris(LiverpoolJohnMooresUniversity)
[email protected], Fergus(Edinburgh) [email protected] [P11]Small, Emma(ARI,LJMU) [email protected], Stephen(Queen'sUniversityBelfast)
[email protected], Anthony(UniversityofSussex)
[email protected] [P07]Smith, Graham(UniversityofBirmingham)
[email protected], Mathew(UCT) [email protected]
[P26]Smith, Matthew(CardiffUniversity)
[email protected] [P07]Smith, P (Wiley-Blackwell) [email protected], Rachel(KeeleUniversity)
[email protected] [P22]Smith, Robert(UniversityofSussex)
[email protected], Russell(DurhamUniversity)
[email protected] [P27]Soechting, Ilona(UniversityofOxford)
[email protected], David(ESA)
[email protected] [P08]Spain, Timothy(UCL) [email protected] [P18,
P28]Speirs, David(DepartmentofPhysics, University
ofStrathclyde) [email protected][P19]
Squitieri, Valentina(UniversityofBristol)[email protected]
Stanway, Elizabeth(UniversityofBristol)[email protected] [P27]
Stark, Craig(UniversityofSt.Andrews)[email protected] [P19]
Steed, Kimberley(UCL-MSSL) [email protected][P24]
Steves, Bonnie(GlasgowCaledonianUniversity)[email protected] [P10]
Stinson, Greg(CentralLancashire)[email protected] [P31, P31]
Strachan, Mel(UKATC) [email protected][P35]
Stroud, Vanessa(FaulkesTelescopeProject/TheOpenUniversity)[email protected]
Subramanian, Srividya(ArmaghObservatory)[email protected] [P24, P29]
Sullivan, Mark(UniversityofOxford)[email protected] [P20]
Sun, Jian(UCL-MullardSpaceScienceLaboratory)[email protected] [P09]
Sutherland, Will(QueenMary, UniversityofLondon) [email protected] [P15,P15]
Sutorius, Eckhard(InstituteforAstronomy, ROE)[email protected] [P15, P10]
Tam, Kuan(UniversityofStAndrews)[email protected]
Tan, BoonKok(UniversityofOxford)[email protected] [P01]
Tanvir, Nial(UniversityofLeicester)[email protected] [Plenary]
Tatton, Bejamin(UniversityofHertfordshire)[email protected] [P27]
Taylor, Matt(EuropeanSpaceAgency)[email protected] [P03]
Taylor, William(RoyalObservatoryEdinburgh)[email protected]
Thomson, Alan(BritishGeologicalSurvey)[email protected] [P18]
Thomson, Edward(UniversityofGlasgow)[email protected] [P11]
Threlfall, James(UniversityofStAndrews)[email protected] [P34]
Tillson, Henry(OxfordUniversity)[email protected]
Tinetti, Giovanna(UCL) [email protected][P35]
Tittley, Eric(U ofEdinburgh, ROE) [email protected], Durgesh(UniversityofCambridge)
[email protected] [P04]Tsiklauri, David(QueenMaryUniversityof
London) [email protected] [P29]Tunnicliffe, Rachel(UniversityofWarwick)
[email protected] [P20]Turkmani, Rim(ImperialCollege)
[email protected] [P19]Turnbull, Katie(LancasterUniversity)
[email protected] [P28]VanDoorsselaere, Tom(UniversityofWarwick)
[email protected] [P14]Vanninathan, Kamalam(KamalamVanninathan)
[email protected] [P29]Vardanyan, Mihran(UniversityofOxford)
[email protected], Santiago(MSSL/UCL)
[email protected] [P04]Verth, Gary(KU Leuven)
[email protected] [P14]Vickers, Hannah(UniversityofLeicester)
[email protected] [P18]Vidotto, Aline(UniversityofStAndrews)
[email protected] [P32]Waldmann, Ingo(UCL) [email protected]
[P12]Walker, Helen(STFC RutherfordAppletonLab)
[email protected] [P33]Walker, Matthew(InstituteofAstronomy,
UniversityofCambridge)[email protected] [P11]
Walker, Simon(UniversityofWarwick)[email protected]
Wallace, Alison(UCL-MSSL) [email protected][P23, P33]
Walsh, Andrew(MSSL-UCL) [email protected][P03]
Walsh, Robert(UniversityofCentralLancashire)[email protected] [P09]
Ward-Thompson, Derek(CardiffUniversity)[email protected] [P07]
Watson, Fraser(UniversityofGlasgow)[email protected] [P34]
Watson, Laura(ImperialCollege, London)
[email protected] [P25]Weidner, Carsten(UniversityofStAndrews)
[email protected], Patrick(JodrellBankCentrefor
Astrophysics)[email protected] [P13]
Wesson, Roger(UniversityCollegeLondon)[email protected] [P12, P07]
Westmoquette, Mark(UCL) [email protected][P31]
Whaler, Kathy(UniversityofEdinburgh)[email protected] [Plenary]
White, Richard(UniversityofLeeds)[email protected] [P35]
Wild, Jim(LancasterUniversity)[email protected] [P18, P33]
Williams, Anthony(UniversityofLeicester)[email protected] [P24, P18]
Williams, David(UCL) [email protected] [P09]Wilmot-Smith, Antonia(UniversityofDundee)
[email protected] [P23, P23]Wilson, Fiona(UniversityofStAndrews)
[email protected] [P23]Woan, Graham(UniversityofGlasgow)
[email protected] [P30, P30, P10]Wood, Alan(AberystwythUniversity)
[email protected] [P18, P13]Wood, Patricia(KeeleUniversity)
[email protected], Emma(LancasterUniversity)
[email protected] [P18]Woods, Paul(UniversityofManchester)
[email protected] [P27]Wright, Andrew(UniversityofStAndrews)
[email protected] [P19]Wright, Gillian(UniversityofEdinburgh)
[email protected] [Plenary]Wu, Xufen(PhysicsandAstronomy, Universityof
StAndrews) [email protected] [P31]Wyper, Peter(Sheffield)
[email protected] [P23]Wyse, Rosie(JohnsHopkinsUniversity)
[email protected] [Plenary]Yates, Japheth(UniversityCollegeLondon)
[email protected] [P08]Yeates, Anthony(UniversityofDundee)
[email protected] [P23, P24]Young, John(UniversityofCambridge)
[email protected] [P22, P22, P22]Young, Neil(UniversityofManchester)
[email protected][P30]
Yu, Shenghua(ArmaghObservatory)[email protected] [P08]
Zhang, ZengHua(UniversityofHertfordshire)[email protected] [P26]
Zhao, Hongsheng(U. ofStAndrews(SUPA))[email protected] [P31, P21, P21]
Zharkov, Sergei(MSSL,UCL) [email protected][P14]
daCosta, AntonioArmando(InstitutoSuperiorTécnico, Lisboa, Portugal)[email protected] [P30]
vanDriel-Gesztelyi, Lidia(MSSL/UCL)[email protected] [P24, P29]
vanSpaandonk, Lieke(UniversityofWarwick)[email protected] [P26]
101
8b9be3970f4d, 2010-04-05T15:25:39+01:00
�������
�
����
������
���
���
�����
��
������
������
�
��
�
�������
��������
�
����
��
�����
���
���
���
����
��
�!��
"�������
Mon 12th
Tue 13thW
ed 14thThu 15th
Fri 16th
����������� ���
�������
������������ �������������
������������� ������
� �������������������� �����
����������
������� ���� !����"�����
�������#���$����
%�������
��������&���� �����"���
�������� ���� �������
"�����
10:20-10:45���
��'���()����������
��'���()����������
��'���()����������
��'���()�������
10:45-12:30��������*������&
+�,-.��,/��������*������
+��-.�&,/��������*������-
+�&-.�,/��������*�������
+��.�0/
12:30-14:0012����������
���+��,,/
�3*45����
"��
���65����*�7
�5�����������5����
8!*�5����
1�������5����)���� �
�����
������������ ���(
�����������
�������0���� "������
'����
�������9���� ����
4��:��
�������&���� '�;5���������-���� 7
����<
��������������
��������,���� '��������*�����2��(���
15:20-15:45���
��'���()����������
��'���()����������
��'���()����������
������()�������
15:45-17:30��������*�������
+�,�.�,0/��������*������
+���.��0/��������*������0
+�&�.�&0/�7
*���������
7=������
12���������2���+�#�,.&,�,,/
������>��<���
+���,.�9�,,/������?
�������+�9�,,.& �,,/
������>��<���
+���,.�9�,,/
0.�.��������;���
��;���4��(@$���'��<�
?5�����
����+�9�,/
Evening*�������������;+&,�,.&�,,/
��;���4��(@�����5�����
+�9�,/��;���4��(@$��
"���
+�9�,/
*������6?1�������
7=������
09:00-10:20
14:00-15:20�7
*���������
7=������
��� �����?
������*���2