thanks for cooperation with dick manchester (atnf, australia), g.j. qiao (pku, china),
DESCRIPTION
Magnetic fields in our Galaxy How much do we know JinLin Han National Astronomical Observatories Chinese Academy of Sciences Beijing, China [email protected]. Thanks for cooperation with Dick Manchester (ATNF, Australia), G.J. Qiao (PKU, China), - PowerPoint PPT PresentationTRANSCRIPT
Magnetic fields in our GalaxyMagnetic fields in our GalaxyHow much do we know How much do we know
JinLin HanJinLin HanNational Astronomical ObservatoriesNational Astronomical Observatories
Chinese Academy of SciencesChinese Academy of Sciences Beijing, ChinaBeijing, [email protected]@bao.ac.cn
Thanks for cooperation with Dick ManchesterDick Manchester (ATNF, Australia), G.J. Qiao G.J. Qiao (PKU, China), A.G. LyneA.G. Lyne (Jodrell Bank, UK), K. Ferriere K. Ferriere (Obs. Midi-Pyr. France)
Galactic B field: Galactic B field: How much How much we we want to knowwant to know
B-StrengthB-Strength1. Random vs. ordered ( <δB>2/B2 )2. Local vs. large-scale B~ f(R)? B~ f(z)?
B-StructureB-Structure 1. Disk field: local 2. Disk: large stru
cture?3. Direction rever
sal in arm or interarm
4. Field in halo?5. Field near GC?
Strength vs. Strength vs. scalesscales
Spatial B-Spatial B-Energy Energy
SpectrumSpectrum
Magnetic fields in our Magnetic fields in our
GalaxyGalaxyHow much do we know ?How much do we know ?
• Some background, remindingSome background, reminding
• Knowledge 10 years agoKnowledge 10 years ago
• Current knowledgeCurrent knowledge– Central field & halo field Central field & halo field
– disk fielddisk field
» directions directions
» strengthstrength
– spatial magnetic energy spectrumspatial magnetic energy spectrum
• What we should know in futureWhat we should know in future
Observational tracers of magnetic fieldsObservational tracers of magnetic fields• Polarization of starlight: perpendicular field in 2 or 3 kpcperpendicular field in 2 or 3 kpc
orientation // B⊥ ------------- 9000 stars
• Zeeman splitting: parallel field, parallel field, in situin situ (masers, clouds) (masers, clouds) △ ∝ B// ------ 30 masers
• Polarization at infrared, mm: perpendicular field perpendicular field orientation // B⊥ ------ clouds & star formation regions
• Synchrotron radiation: vertical field structures (added)vertical field structures (added)
total intensity S ∝ B⊥2/7, p% B∝ ⊥u
2 / B t⊥2
• Faraday rotation: parallel field, integrated (the halo & disk)parallel field, integrated (the halo & disk)
RM ∝ ∫ ne B// ds ------ 500 pulsars + >1000 EGSes
• 9000 stars have polarization measured• mostly nearby (1~2kpc)• polarization percentage increases with distance
Zweibel & Heiles 1997, Nature 385,131 Berdyugin & Teerikorpi 2001, A&A 368,635
Starlight polarization:Starlight polarization: local field // armlocal field // arm
Zeeman Effect: Zeeman Effect: B in molecular cloudsB in molecular clouds
Bourke et al. 2001, ApJ 554, 916
>30 people working for >30 people working for >30 years, get>30 years, get
<30 good measurements!<30 good measurements!
Difficult &Difficult & Bad Luck!Bad Luck!
Maser B-fields: Nothing to do with large-scale B-field?!Nothing to do with large-scale B-field?!
ne: ISM: 1cm-3 ==> GMC: 103cm-3
==> OH-maser: 107cm-3
Fish et al. 2003
Reid & Silverstein 1990, ApJ 361, 483
41 clockwise33 counterclockwiseAssume Bφ>> Br or Bz
Observational tracers of magnetic fieldsObservational tracers of magnetic fields• Polarization of starlight: perpendicular field in 2 or 3 kpcperpendicular field in 2 or 3 kpc
orientation // B⊥ ------------- 9000 stars
• Zeeman splitting: parallel field, in situ (masers, clouds)parallel field, in situ (masers, clouds) △ ∝ B// ------ 30 masers
• Polarization at infrared, mm: perpendicular field perpendicular field orientation // B⊥ ------------- star formation regions
• Synchrotron radiation: vertical field structures (added)vertical field structures (added)
total intensity S ∝ B⊥2/7, p% B∝ ⊥u
2 / B t⊥2
• Faraday rotation: parallel field, integrated (the halo & disk)parallel field, integrated (the halo & disk)
RM ∝ ∫ ne B// ds ------ 500 pulsars + >1000 EGSes
Polarization at mm, sub-mm, infraredWorking toward measure B-field of galactic scale
• thermal emission (of dusts)• aligned by B-field in the clouds
Hildebrand et al. PASP 112, 1215
Synchrotron radiation: transverse B-structurestransverse B-structuresGlobal B-field structure from linearly polarized emission
How to distinguish?How to distinguish?
RM maps helps on directions of RM maps helps on directions of (disk &) halo field!(disk &) halo field!
MPIFR has a group working on MPIFR has a group working on this for 25 years!this for 25 years!
No information of B-directions!
Han et al. 1999, A&A 384, 405
Two Possible origin of polarization:
• Large-scale magnetic field as vectors shown (convention)Large-scale magnetic field as vectors shown (convention)• Anisotropic random field compressed by large-scale density waveAnisotropic random field compressed by large-scale density wave
Observational tracers of magnetic fieldsObservational tracers of magnetic fields• Polarization of starlight: perpendicular field in 2 or 3 kpcperpendicular field in 2 or 3 kpc
orientation // B⊥ ------------- 9000 stars
• Zeeman splitting: parallel field, in situ (masers, clouds)parallel field, in situ (masers, clouds) △ ∝ B// ------ 30 masers
• Polarization at infrared, mm : perpendicular field perpendicular field orientation // B⊥ ------------- star formation regions
• Synchrotron radiation : vertical field structures (added)vertical field structures (added)
total intensity S ∝ B⊥2/7, p% B∝ ⊥u
2 / B t⊥2
• Faraday rotation: parallel field, integrated (the halo & disk)parallel field, integrated (the halo & disk)
RM ∝ ∫ ne B// ds ------ 500 pulsars + >1000 EGSes
Pulsars: Best probes for Large-scale Galactic B-field
• Widely distributed in GalaxyWidely distributed in Galaxy• Distance from DM: Distance from DM: 3-D3-D B-field B-field• Linearly polarized: RM easy to obsLinearly polarized: RM easy to obs• No intrinsic RMs: No intrinsic RMs: Direct <B>Direct <B>
Pulsar distribution
Why? Pulsars as probes for Galactic B-field• Polarized. Widely spread in our Galaxy. Faraday rotation:
• Distances estimated from pulse dispersion:
» <===<=== the delay tells DM»
» the rotation of position» angles tells RM value ===>===>
» Average field strength is
0
Dist
eDM n dl
sec103.83
3
MHz
DMt
22
21
21
PAPA
RM
GDM
RMB 232.1=
Dist
e
PSR
Sunobs
ee
dlnBdll
lBlncm
eRM
0||2
||42
3
820.0])(
)[()(2
• Ordered:Ordered: irregular (random) + regular (uniform)
• Line of sight:Line of sight: perpendicular + parallel
• StructuralStructuraltoroidal (azimuthal) + poloidal (vertical)
• LocationsLocationsLocalized features &/or Global structure
Just remind you ……
Magnetic field should have complicated structure, but often is
artificially said to have components of
Our Milky Way Galaxy: What structure? Our Milky Way Galaxy: What structure?
• Our Galaxy: we live near the we live near the
edgeedge
• We do not knowdo not know the structure
of our own Galaxy
• We want to work out (via We want to work out (via
radio view)radio view) how its magnetic
field looks like, and where it
originates from?
Optical sky
Radio sky
• how many spiral arms: 2 or 4, or 3?• pitch angle of spiral: 8o, 10o or 14o ?
KnowledgeKnowledge ofof
10 years ago ……10 years ago ……
• disk field:disk field:
* 3 models * which one?which one?
Concentric Rings Axi-symmetric Bi-Symmetric Spiral Concentric Rings Axi-symmetric Bi-Symmetric Spiral
Rings model spiral (ASS) (BSS)Rings model spiral (ASS) (BSS)
Galactic magnetic fields: 10 years Galactic magnetic fields: 10 years agoago
• Halo field:Halo field:
* no idea on halo fieldno idea on halo field * Poloidal fieldsPoloidal fields near GC:near GC: YesYes
see see nonthermal filamentsnonthermal filaments
Axi-Symmetric Spiral model by J.P. Vallee• Main Problem: fields go across the arms• Just one Just one radius radius range for reversedrange for reversed fields fields• Not consistent with field reversals near -- Perseus arm???? -- the Norma arm !!the Norma arm !!
BSS reversalBSS reversalBSS reversal
?
?
Ring model: Concentric rings of reversed fields• Selection effect problem ??Selection effect problem ??• Field lines go across the arms?Field lines go across the arms?• Inconsistent Formula for the BSS when Inconsistent Formula for the BSS when
modeling ??modeling ??It is the zero-order modelling only fIt is the zero-order modelling only f
or azimuthal magnetic field !or azimuthal magnetic field !
by R. Rand & S. Kulkarni (1989)
R. Rand & A.Lyne(1994)
There were not as many pulsar RMs as today….There were not as many pulsar RMs as today….
Bi-Symmetric Spiral ModelBi-Symmetric Spiral ModelProposed from RMs of
Extragalactic Radio Sources:
Simard-Normandin & Kronberg (1980)
Sofue & Fujimoto (1983)
Confirmed by Pulsar RMs: Han & Qiao (1994) Indrani & Deshpande (1998) Han, Manchester, Qiao (1999) Han,Manchester, Lyne, Qiao(2002)
Supported by starlight polarization
Heiles (1996)
The best match to all evidenceThe best match to all evidence field reversals & pitch angle – 8°±2°( the field stronger in interarm region ? ? ? ? )
Current knowledge ……Current knowledge ……•Central field & halo field Central field & halo field •disk field: disk field: directions & Strengthdirections & Strength•magnetic energy spectrummagnetic energy spectrum
Poloidal & Toroidal fields near GCPoloidal & Toroidal fields near GCToroidal fieldsToroidal fields
(Novak et al. 2003, 2000)• permeated in the central molecular zonecentral molecular zone (400pc*50pc)(400pc*50pc)
• sub-mm obs of p%• toroidal field directions determined by averaged RMs of plumes or SNR!
Poloidal fieldPoloidal field filaments Unique to GC --- dipolar geometry! (Morris 1994; Lang et al.1999)
(from Novak et al. 2003)
150pc
GC
Predicted B-direction
Magnetic fields in our Galaxy: near GCnear GC
Spiral arms & B- fields continue near GC?
– Yes in NGC 2997 (Han et al. 1999)–- How strong?
Poloidal fields– reason for jets?– dipole field?– related to vertical-B?– how strong?
(from B.D.C. Chandran 2000)
Optical sky
Radio sky
To study halo field: unique to our Galaxyunique to our Galaxy
• The largest edge-on Galaxy in the sky
• Pulsars and extragalactic radio sources as probes
PulsarsRM distribution
• The largest edge-on Galaxy in the sky
• Pulsars and extragalactic radio sources as probes
Extragalactic Radio SourcesExtragalactic Radio Sources RM distribution
To study halo field: unique to our Galaxyunique to our Galaxy
<B> away from usRM<0
RM>0<B> to us
Anti-symmetric RM sky: Anti-symmetric RM sky: A0 dynamoA0 dynamo (Han et al. 1997 A&A322, (Han et al. 1997 A&A322, 98)98)
Evidence for global scale
• High anti-symmetry to the
Galactic coordinates
• Only in inner Galaxy
• nearby pulsars show it at
higher latitudes
Implications
• Consistent with field
configuration of A0
dynamo
• The first dynamo mode The first dynamo mode
identified on galactic identified on galactic
scalesscales
Bv
Unique measurement
of Vertical B-component
Bv = 0.
2 ~ 0.3G pointing from SGP to NGP (Effect of the NPS discounted already!)
Local vertical components: fromLocal vertical components: from poloidal field?poloidal field?
South Galactic Pole
North Galactic Pole
(see Han & Qiao 1994; Han et al. 1999)
Magnetic field configurations for basic dynamos
M31: only 21 polarized brightbackground sources available !!
Han, Beck, Berkhuijsen (1998):
An even mode (S0) dynamo may operate in M31 !
A0
S0
S1
Current knowledge ……Current knowledge ……•Central field & halo field Central field & halo field •disk field: disk field:
»directions directions »StrengthStrength
•magnetic energy spectrummagnetic energy spectrum
Bi-Symmetric Spiral ModelBi-Symmetric Spiral ModelProposed from RMs of
Extragalactic Radio Sources:
Simard-Normandin & Kronberg (1980)
Sofue & Fujimoto (1983)
Confirmed by Pulsar RMs: Han & Qiao (1994) Indrani & Deshpande (1998) Han, Manchester, Qiao (1999) Han,Manchester, Lyne, Qiao(2002)
Supported by starlight polarization
Heiles (1996)
The best match to all evidenceThe best match to all evidence field reversals & pitch angle – 8°±2°( the field stronger in interarm region ? ? ? ? )
CCW B-field along the Norma arm: from New Pulsar RMs
possible field directions
Field directions newly
determined
Han et al. 2002, ApJ 570, L17Han et al. 2002, ApJ 570, L17
Coherent B-fieldB-field directionsdirections >5 kpc along Norma ar
m
Another reversed field in large-sclarge-sc
aleale?
????
Large-scale magnetic field in the Galactic disk
The largest The largest coherentcoherent field structrue detected in the Universe! field structrue detected in the Universe!
How to distinguish?How to distinguish?
RM maps helps on directions of RM maps helps on directions of (disk &) halo field!(disk &) halo field!
MPIFR has a group working on MPIFR has a group working on this for 25 years!this for 25 years!
No information of B-directions!
Synchrotron radiation: transverse B-structurestransverse B-structuresGlobal B-field structure from linearly polarized emission
Han et al. 1999, A&A 384, 405
Two possible reasons for polarization of Synchrotron radiation ofSynchrotron radiation of External Galaxies:External Galaxies:
• Large-scale magnetic field as vectors shown (conventionally)Large-scale magnetic field as vectors shown (conventionally)• Anisotropic random fieldAnisotropic random field compressed by large-scale density wave compressed by large-scale density wave
Polarized radio mission origins fromPolarized radio mission origins from
large-scale uniform field?large-scale uniform field?
Based on pulsar data in oBased on pulsar data in o
ur galaxy <B>=RM/DM:ur galaxy <B>=RM/DM:
YES!YES! But maybeBut maybe partially partially
Han et al. 2002 ApJ 570, L17Han et al. 2002 ApJ 570, L17
Current knowledge ……Current knowledge ……•Central field & halo field Central field & halo field •disk field: disk field:
»directionsdirections »StrengthStrength
•magnetic energy spectrummagnetic energy spectrum
Current knowledge ……Current knowledge ……•Central field & halo field Central field & halo field •disk field: disk field: directions & Strengthdirections & Strength•magnetic energy spectrummagnetic energy spectrum
Why our Galaxy has magnetic field?Why our Galaxy has magnetic field?
Probably Dynamo!Probably Dynamo!
How dynamo works? How dynamo works?
Alpha-Omega effect.Alpha-Omega effect.
Dynamo Really works?Dynamo Really works?
Computer SimulationsComputer Simulations….….
Many Simulations of dynamosMany Simulations of dynamos---- ---- check spacial B-energy spectrum & its evolution check spacial B-energy spectrum & its evolution e.g. Magnetic energy distribution on different spatial scalese.g. Magnetic energy distribution on different spatial scales (k=1/λ) (k=1/λ)
Many papers by Many papers by • N.E. L. Haugen, A. Brandenburg, W. Dobler, …..N.E. L. Haugen, A. Brandenburg, W. Dobler, …..• A. Schekochihin, S.C. Cowley, S. Taylor, J. Moron, ….. A. Schekochihin, S.C. Cowley, S. Taylor, J. Moron, ….. • E. Blackman, J. Maron …..E. Blackman, J. Maron …..• Others …..Others …..
No real measurements No real measurements
to check whether to check whether
dynamo works or not! dynamo works or not!
Far away from telling anything about a real galaxy ……Far away from telling anything about a real galaxy ……
Don’t know much about the large-scale magnetic Don’t know much about the large-scale magnetic field ...field ...
What spatial magnetic energy spectrum What spatial magnetic energy spectrum
does does our Galaxy have?our Galaxy have?
Spatial fluctuation spectrum for electron densitySpatial fluctuation spectrum for electron density
““The Big Powerlaw in the SkyThe Big Powerlaw in the Sky””
B-field & electrons B-field & electrons
coupling? If so, coupling? If so,
B-energy spectrum?B-energy spectrum?
KolmogorovKolmogorovover 12 orderover 12 orders in scale?s in scale?
10 pc
1000 km
(Armstrong, Rickett & Spangler 1995)
Minter & Spangler 1996Minter & Spangler 1996
Spacial energy spectrum of B PreviouslyPreviously only only available information from available information from RM structure function RM structure function
λ< ~4pc: consistent to Kolmogorov 3D 80>λ> ~4pc: turbulence in 2D?
Pulsar RM distribution in Galactic planered: new measurements by Parkes 64m telescope
PSR
Sun e dllBlnRM )()( ||
Spatial magnetic energy spectrum of our GalaxySpatial magnetic energy spectrum of our Galaxy (Han et al. 2004, ApJ 610, 820)(Han et al. 2004, ApJ 610, 820)
Minter & Spangler Minter & Spangler 19961996
By pulsar By pulsar
RM/DMRM/DM
Email from A. MinterEmail from A. Minter
Conclusive Remarks Conclusive Remarks More data neededMore data needed ---- Best we can say Best we can say up to nowup to now • Halo field
• Disk field
• Spatial Energy spectrum
• Radial Radial DependenceDependence(unpublished)(unpublished)
If I have time, I tell you more aboutwhat we are doing ……
Thanks for your attention.Thanks for your attention.
Current doing & future ……Current doing & future ……
• Halo field: structure and field strengthHalo field: structure and field strength
• What difference: What difference:
fields in arm and interarmfields in arm and interarm
• Structure in large regions: More pulsars?Structure in large regions: More pulsars?
• Structure in more detailsStructure in more details
• Field in intergalactic spaceField in intergalactic space
RMs of EGRs for the halo B-field RMs of EGRs for the halo B-field Only about 1000 ROnly about 1000 RMs available in literMs available in literature upto now...ature upto now...
We are using EffelWe are using Effelsberg -100m telescsberg -100m telescope to make a RM ope to make a RM survey of 1700 sousurvey of 1700 sources, enlarge the crces, enlarge the cover density by a fover density by a factor of three in moactor of three in most sky area……st sky area……
Difference for RMs of PSRs & EGResDifference for RMs of PSRs & EGRes
Galactic plane polarization survey at 6cmGalactic plane polarization survey at 6cm
Urumqi 25m telescope
MPIfR 6cm receiver
Just messioned last week…. Will finish in 3 years ...Just messioned last week…. Will finish in 3 years ...
• Cooperation withCooperation with MPIfRMPIfR• System hardwareSystem hardware & software& software almost okalmost ok• No data at this No data at this frequencyfrequency• Less affacted by Less affacted by foreground RMforeground RM• Useful for CMB Useful for CMB polarizationpolarization
总强度图总强度图 偏振强度图偏振强度图
Field reversals exterior to the PField reversals exterior to the Perseus arm -- it is fine!erseus arm -- it is fine!Brown et al. 2003, ApJ 593, L29Mitra et al. 2003, A&A 398,993
Han et al. 1999
Han et al. 1999Lyne & Smith 1989
Evidence at 150<l<100 is very weak, butEvidence at 150<l<100 is very weak, butEvidence for Evidence for two reversalstwo reversals at l~70 is hard! at l~70 is hard!
Field reversals exterior to the Perseus armField reversals exterior to the Perseus arm
Han et al. 1999
Weisberg et al. 2004
Will be checked byWill be checked by
RMs of RMs of ALFA PSRsALFA PSRs
(to be discovered!)(to be discovered!)
Field strength & B-energy vs. Distance/scalesField strength & B-energy vs. Distance/scales(Han et al. 2004, ApJ 610, 820)(Han et al. 2004, ApJ 610, 820)