georg raffelt, max-planck-institut für physik, münchen physik kolloquium, 19. november 2007, rwth...

Georg Raffelt, Max-Planck-Institut für Physik, München Physik Kolloquium, 19. November 2007, RWTH Aachen

TitleTitle

Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen

Physik Kolloquium,Physik Kolloquium, 19.19. November 2007November 2007

RWTH AachenRWTH AachenExzellenzExzellenz


Aachen SkylineAachen Skyline

Supernova Neutrinos20 Years after SN 1987A


Sanduleak Sanduleak 69 69 202202

Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc (160.000 light years)(160.000 light years)

Tarantula NebulaTarantula Nebula

Supernova 1987ASupernova 1987A 23 February 198723 February 1987



Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A



Crab NebulaCrab Nebula



Supernova 1054 PetrographSupernova 1054 Petrograph

Possible SN 1054 Petrograph by the Anasazi peoplePossible SN 1054 Petrograph by the Anasazi people(Chaco Canyon, New Mexico)(Chaco Canyon, New Mexico)

CrescentCrescentMoonMoon

3 concentric circles, 3 concentric circles, diameter diameter 1 foot, 1 foot, with huge red flameswith huge red flamestrailing to the right.trailing to the right.(Halley’s Comet(Halley’s Comet ?)?)

SN 1054SN 1054

Hand signifiesHand signifiessacred placesacred place


Helium-burning starHelium-burning star

HeliumHeliumBurningBurning

HydrogenHydrogenBurningBurning

Main-sequence starMain-sequence star

Hydrogen BurningHydrogen Burning

Onion structureOnion structure

Degenerate iron core:Degenerate iron core: 101099 g cm g cm33

T T 10 1010 10 K K

MMFeFe 1.5 M 1.5 Msunsun

RRFeFe 8000 km 8000 km

Collapse (implosion)Collapse (implosion)

Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion


Collapse (implosion)Collapse (implosion)ExplosionExplosionNewborn Neutron StarNewborn Neutron Star

~ 50 km~ 50 km

Proto-Neutron StarProto-Neutron Star

nucnuc 3 3 10101414 g cm g cm33

T T 30 MeV 30 MeV

NeutrinoNeutrinoCoolingCooling



Newborn Neutron StarNewborn Neutron Star

~ 50 km~ 50 km

Proto-Neutron StarProto-Neutron Star

nucnuc 3 3 10101414 g cm g cm33

T T 30 MeV 30 MeV

NeutrinoNeutrinoCoolingCooling

Gravitational binding energyGravitational binding energy

EEbb 3 3 10 105353 erg erg 17% M 17% MSUN SUN cc22

This shows up as This shows up as 99% Neutrinos99% Neutrinos 1% Kinetic energy of explosion1% Kinetic energy of explosion (1% of this into cosmic rays) (1% of this into cosmic rays) 0.01% Photons, outshine host galaxy0.01% Photons, outshine host galaxy

Neutrino luminosityNeutrino luminosity

LL 3 3 10 105353 erg / 3 sec erg / 3 sec

3 3 10 101919 L LSUNSUN

While it lasts, outshines the entireWhile it lasts, outshines the entire visible universevisible universe



Periodic System of Elementary ParticlesPeriodic System of Elementary Particles

QuarksQuarks LeptonsLeptons

Charge Charge 2/3 2/3

Up Up

Charge Charge 1/3 1/3

Down Down

Charge Charge 1 1

Electron Electron

Charge Charge 00

e-Neutrino e-Neutrino eeeedduu

NeutronNeutron

ProtonProton

QuarksQuarks LeptonsLeptons

Charm Charm

Top Top

Gravitation Gravitation

Weak InteractionWeak Interaction

Strong Interaction (QCD)Strong Interaction (QCD)

Electromagnetic Interaction (QED)Electromagnetic Interaction (QED)

Down Down

Strange Strange

Bottom Bottom

Electron Electron

Muon Muon

Tau Tau

e-Neutrino e-Neutrino

-Neutrino -Neutrino

1st Family1st Family

2nd Family 2nd Family

3rd Family3rd Family

Charge Charge 2/3 2/3 Charge Charge 1/3 1/3 Charge Charge 1 1 Charge Charge 00

Up Up

-Neutrino -Neutrino

eeee

dd

ss

bb

cc

tt

uu


Where do Neutrinos Appear in Nature?Where do Neutrinos Appear in Nature?

AstrophysicalAstrophysicalAccelerators Accelerators Soon ?Soon ?

Cosmic Big Bang Cosmic Big Bang (Today 330 (Today 330 /cm/cm33)) Indirect EvidenceIndirect Evidence

Nuclear ReactorsNuclear Reactors

Particle AcceleratorsParticle Accelerators

Earth AtmosphereEarth Atmosphere(Cosmic Rays)(Cosmic Rays)

SunSun

SupernovaeSupernovae(Stellar Collapse)(Stellar Collapse)

SN 1987ASN 1987A

Earth Crust Earth Crust (Natural (Natural Radioactivity)Radioactivity)


Hans Bethe (1906Hans Bethe (19062005, Nobel prize 1967)2005, Nobel prize 1967)Thermonuclear reaction chains (1938)Thermonuclear reaction chains (1938)

Neutrinos from the SunNeutrinos from the Sun

Solar radiation: 98 % lightSolar radiation: 98 % light 2 % neutrinos2 % neutrinosAt Earth 66 billion neutrinos/cmAt Earth 66 billion neutrinos/cm22 sec sec

Reaction-Reaction-chainschains

EnergyEnergy26.7 MeV26.7 MeV

HeliumHelium


Sun Glasses for Neutrinos?Sun Glasses for Neutrinos?

Several light years of lead Several light years of lead needed to shield solarneeded to shield solar neutrinosneutrinos

Bethe & Peierls 1934:Bethe & Peierls 1934: “… “… this evidently meansthis evidently means that one will never be ablethat one will never be able to observe a neutrino.”to observe a neutrino.”

8.3 light minutes8.3 light minutes


First Detection (1954 -First Detection (1954 - 1956)1956)

Fred ReinesFred Reines(1918 – 1998)(1918 – 1998)

Nobel prize 1995Nobel prize 1995

Clyde CowanClyde Cowan(1919 – 1974)(1919 – 1974)

Detector prototypeDetector prototype

Anti-Electron Anti-Electron NeutrinosNeutrinosfrom from Hanford Hanford Nuclear ReactorNuclear Reactor

3 Gammas3 Gammasin coincidencein coincidenceee pppp

nnnn CdCdCdCd

ee++ee++ ee--ee--


Inverse beta decayInverse beta decayof chlorineof chlorine

600 tons of600 tons ofPerchloroethylenePerchloroethylene

Homestake solar neutrinoHomestake solar neutrino observatory (1967observatory (19672002)2002)

First Measurement of Solar NeutrinosFirst Measurement of Solar Neutrinos


Cherenkov EffectCherenkov EffectCherenkov EffectCherenkov Effect

WaterWater

Elastic Elastic scattering or CC scattering or CC

reactionreaction

Neutrino

NeutrinoLightLight

LightLight

CherenkCherenkov Ringov Ring

Electron or MuonElectron or Muon(Charged Particle)(Charged Particle)



Super-Kamiokande Neutrino DetectorSuper-Kamiokande Neutrino Detector

42 m42 m

39.3 39.3 mm


Cherenkov RingCherenkov Ring



Super-Kamiokande: Sun in the Light of Super-Kamiokande: Sun in the Light of NeutrinosNeutrinos



SN 1987A Event No.9 in Kamiokande-II SN 1987A Event No.9 in Kamiokande-II

Kamiokande-II detectorKamiokande-II detector2140 tons of water fiducial volume2140 tons of water fiducial volumefor SN 1987Afor SN 1987A

Hirata et al., PRD 38 (1988) 448Hirata et al., PRD 38 (1988) 448


Neutrino Signal of Supernova 1987ANeutrino Signal of Supernova 1987A

Within clock uncertainties,Within clock uncertainties,signals are contemporaneoussignals are contemporaneous

Kamiokande-II (Japan)Kamiokande-II (Japan)Water Cherenkov detectorWater Cherenkov detector2140 tons2140 tonsClock uncertainty Clock uncertainty 1 min1 min

Irvine-Michigan-Brookhaven (US)Irvine-Michigan-Brookhaven (US)Water Cherenkov detectorWater Cherenkov detector6800 tons6800 tonsClock uncertainty Clock uncertainty 50 ms50 ms

Baksan Scintillator TelescopeBaksan Scintillator Telescope(Soviet Union), 200 tons(Soviet Union), 200 tonsRandom event cluster ~ 0.7/dayRandom event cluster ~ 0.7/dayClock uncertainty +2/-54 sClock uncertainty +2/-54 s


2002 Physics Nobel Prize for Neutrino 2002 Physics Nobel Prize for Neutrino AstronomyAstronomy

Ray Davis Jr.Ray Davis Jr.(1914 (1914 2006)2006)

Masatoshi KoshibaMasatoshi Koshiba(*1926)(*1926)

““for pioneering contributions to astrophysics, in for pioneering contributions to astrophysics, in particular for the detection of cosmic neutrinos”particular for the detection of cosmic neutrinos”




Some Particle-Physics Some Particle-Physics Lessons from SN 1987ALessons from SN 1987A


The Energy-Loss ArgumentThe Energy-Loss Argument

NeutrinoNeutrinospheresphere

NeutrinoNeutrino diffusiondiffusion

Late-time signal most sensitive observableLate-time signal most sensitive observable

Emission of very weakly interactingEmission of very weakly interactingparticles would “steal” energy from theparticles would “steal” energy from theneutrino burst and shorten it.neutrino burst and shorten it.(Early neutrino burst powered by accretion,(Early neutrino burst powered by accretion, not sensitive to volume energy loss.)not sensitive to volume energy loss.)

Volume emissionVolume emission of novel particlesof novel particles

SN 1987A neutrino signalSN 1987A neutrino signal


Neutrino Limits by Intrinsic Signal DispersionNeutrino Limits by Intrinsic Signal Dispersion

Time of flight delay by neutrino massTime of flight delay by neutrino mass (G. Zatsepin, JETP Lett. 8:205, 1968) (G. Zatsepin, JETP Lett. 8:205, 1968)

mmee ≲≲ 20 eV20 eV

• At the time of SN 1987A At the time of SN 1987A competitive with tritium end-pointcompetitive with tritium end-point

• Today mToday m << 2.2 eV from tritium 2.2 eV from tritium

• Cosmological limit today mCosmological limit today m ≲≲ 0.2 eV 0.2 eV

22

eV10m

EMeV10

kpc50D

s57.2t

22

eV10m

EMeV10

kpc50D

s57.2t

For “milli charged” For “milli charged” neutrinos, neutrinos, pathpath bent by galactic magnetic field, bent by galactic magnetic field, inducing a time delayinducing a time delay

Assuming charge conservation inAssuming charge conservation inneutron decay yields a moreneutron decay yields a morerestrictive limit of about 3restrictive limit of about 310102121 e e

122

2B

2103

E6

)dB(ett

12

2

2B

2103

E6

)dB(ett

B

17dkpc1

BG1

103e

e

B

17dkpc1

BG1

103e

e

• Barbiellini & Cocconi,Barbiellini & Cocconi, Nature 329 (1987) 21Nature 329 (1987) 21• Bahcall, Neutrino Astrophysics (1989)Bahcall, Neutrino Astrophysics (1989)

Loredo & LambLoredo & LambAnn N.Y. Acad. Sci. 571 (1989) 601Ann N.Y. Acad. Sci. 571 (1989) 601find 23 eV (95% CL limit) from detailedfind 23 eV (95% CL limit) from detailedmaximum-likelihood analysismaximum-likelihood analysis


Do Neutrinos Gravitate?Do Neutrinos Gravitate?

Neutrinos arrive a few hours earlier than photons Neutrinos arrive a few hours earlier than photons Early warning (SNEWS) Early warning (SNEWS)SN 1987A: Transit time for photons and neutrinos equal to within ~ 3hSN 1987A: Transit time for photons and neutrinos equal to within ~ 3h

Equal within ~ 1 Equal within ~ 1 4 4 101033

Shapiro time delay for particles moving in a Shapiro time delay for particles moving in a gravitational potential gravitational potential

Longo, PRL 60:173,1988Longo, PRL 60:173,1988Krauss & Tremaine, PRL 60:176,1988Krauss & Tremaine, PRL 60:176,1988

• Proves directly that neutrinos respond to gravity in the usual wayProves directly that neutrinos respond to gravity in the usual way because for photons gravitational lensing already proves this pointbecause for photons gravitational lensing already proves this point

• Cosmological limits Cosmological limits NN ≲≲ 1 much worse test of neutrino gravitation 1 much worse test of neutrino gravitation

• Provides limits on parameters of certain non-GR theories of gravitationProvides limits on parameters of certain non-GR theories of gravitation• Photons likely obscured for next galactic SN, so this result probablyPhotons likely obscured for next galactic SN, so this result probably unique to SN 1987A unique to SN 1987A

months51dt)]t(r[U2t BAShapiro months51dt)]t(r[U2t BAShapiro




Core-CollapseCore-CollapseExplosion MechanismExplosion Mechanism


Delayed ExplosionDelayed Explosion

Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys.(1982)Wilson, Proc. Univ. Illinois Meeting on Num. Astrophys.(1982)Bethe & Wilson, ApJ 295 (1985) 14Bethe & Wilson, ApJ 295 (1985) 14


Neutrino-Driven Delayed ExplosionNeutrino-Driven Delayed Explosion

Picture adapted from Janka, astro-ph/0008432Picture adapted from Janka, astro-ph/0008432

Neutrino heatingNeutrino heatingincreases pressureincreases pressurebehind shock frontbehind shock front


Standing Accretion Shock Instability (SASI)Standing Accretion Shock Instability (SASI)Mezzacappa et al., http://www.phy.ornl.gov/tsi/pages/simulations.htmlMezzacappa et al., http://www.phy.ornl.gov/tsi/pages/simulations.html





Galactic Supernova RateGalactic Supernova Rate


Core-Collapse SN Rate in the Milky WayCore-Collapse SN Rate in the Milky Way

Gamma rays fromGamma rays from2626Al (Milky Way)Al (Milky Way)

Historical galacticHistorical galacticSNe (all types)SNe (all types)

SN statistics inSN statistics inexternal galaxiesexternal galaxies

No galacticNo galacticneutrino burstneutrino burst

Core-collapse SNe per centuryCore-collapse SNe per century00 11 22 33 44 55 66 77 88 99 1010

van den Bergh & McClure (1994)van den Bergh & McClure (1994)

Cappellaro & Turatto (2000)Cappellaro & Turatto (2000)

Diehl et al. (2006)Diehl et al. (2006)

Tammann et al. (1994)Tammann et al. (1994)Strom (1994)Strom (1994)

90 90 %% CL (25 y obserservation) CL (25 y obserservation) Alekseev et al. (1993)Alekseev et al. (1993)

References: van den Bergh & McClure, ApJ 425 (1994) 205. Cappellaro & References: van den Bergh & McClure, ApJ 425 (1994) 205. Cappellaro & Turatto, astro-ph/0012455. Diehl et al., Nature 439 (2006) 45. Strom, Astron. Turatto, astro-ph/0012455. Diehl et al., Nature 439 (2006) 45. Strom, Astron. Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekeseev et al., Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekeseev et al., JETP 77 (1993) 339 and my update.JETP 77 (1993) 339 and my update.


Local Group of GalaxiesLocal Group of Galaxies

250250

6060

3030

Events in a detector withEvents in a detector with 30 x Super-K fiducial volume,30 x Super-K fiducial volume, e.g. Hyper-Kamiokandee.g. Hyper-Kamiokande


Nearby Galaxies with Many Observed Nearby Galaxies with Many Observed SupernovaeSupernovae

M83 (NGC 5236, Southern Pinwheel)M83 (NGC 5236, Southern Pinwheel)D = 4.5 MpcD = 4.5 Mpc

Observed Supernovae: Observed Supernovae: 1923A, 1945B, 1950B,1923A, 1945B, 1950B, 1957D, 1968L, 1983N 1957D, 1968L, 1983N

NGC 6946 NGC 6946 D = (5.5 ± 1) MpcD = (5.5 ± 1) Mpc

Observed Supernovae:Observed Supernovae: 1917A, 1939C, 1948B, 1968D,1917A, 1939C, 1948B, 1968D, 1969P, 1980K, 2002hh, 2004et1969P, 1980K, 2002hh, 2004et




Future SupernovaFuture SupernovaNeutrino ObservationsNeutrino Observations


Large Detectors for Supernova NeutrinosLarge Detectors for Supernova Neutrinos

Super-Kamiokande (10Super-Kamiokande (1044))KamLAND (400)KamLAND (400)

MiniBooNEMiniBooNE(200)(200)

In brackets eventsIn brackets eventsfor a “fiducial SN”for a “fiducial SN”at distance 10 kpcat distance 10 kpc

LVD (400)LVD (400)Borexino (100)Borexino (100)

IceCube (10IceCube (1066))

BaksanBaksan (100)(100)


SSuperuperNNova ova EEarly arly WWarning arning SSystem (SNEWS)ystem (SNEWS)

Neutrino observation can alert astronomersNeutrino observation can alert astronomersseveral hours in advance to a supernova.several hours in advance to a supernova.To avoid false alarms, require alarm from atTo avoid false alarms, require alarm from atleast two experiments.least two experiments.

CoincidenceCoincidenceServer Server @ BNL@ BNL

Super-KSuper-K

AlertAlert

Others ?Others ?

LVDLVD

IceCubeIceCube

http://snews.bnl.govhttp://snews.bnl.govastro-ph/0406214astro-ph/0406214

Supernova 1987ASupernova 1987AEarly Light CurveEarly Light Curve


Simulated Supernova Signal at Super-Simulated Supernova Signal at Super-KamiokandeKamiokande

Simulation for Super-Kamiokande SN signal at 10 kpc,Simulation for Super-Kamiokande SN signal at 10 kpc,based on a numerical Livermore modelbased on a numerical Livermore model

[Totani, Sato, Dalhed & Wilson, ApJ 496 (1998) 216][Totani, Sato, Dalhed & Wilson, ApJ 496 (1998) 216]

AccretioAccretionn

PhasePhase

Kelvin-Kelvin-HelmholtzHelmholtz

Cooling PhaseCooling Phase


IceCube Neutrino Telescope at the South PoleIceCube Neutrino Telescope at the South Pole

• 1 km1 km33 antarctic ice, instrumented antarctic ice, instrumented with 4800 photomultiplierswith 4800 photomultipliers• 22 of 80 strings installed (2007)22 of 80 strings installed (2007)• Completion until 2011 foreseenCompletion until 2011 foreseen


IceCube as a Supernova Neutrino DetectorIceCube as a Supernova Neutrino Detector

Each optical module (OM) picks upEach optical module (OM) picks upCherenkov light from its neighborhood.Cherenkov light from its neighborhood.SN appears as “correlated noise”.SN appears as “correlated noise”.

• About 300About 300 CherenkovCherenkov photons photons per OMper OM from a SNfrom a SN at 10 kpcat 10 kpc

• NoiseNoise per OMper OM < 260 Hz< 260 Hz

• Total ofTotal of 4800 OMs4800 OMs in IceCubein IceCube

IceCube SN signal at 10 kpc, basedIceCube SN signal at 10 kpc, basedon a numerical Livermore modelon a numerical Livermore model[Dighe, Keil & Raffelt, hep-ph/0303210][Dighe, Keil & Raffelt, hep-ph/0303210]

Method first discussed byMethod first discussed by• Pryor, Roos & Webster,Pryor, Roos & Webster, ApJ 329:355 (1988)ApJ 329:355 (1988)• Halzen, Jacobsen & ZasHalzen, Jacobsen & Zas astro-ph/9512080astro-ph/9512080


LAGUNA - Funded FP7 Design StudyLAGUNA - Funded FP7 Design Study

LLarge arge AApparati for pparati for GGrand rand UUnification and nification and NNeutrino eutrino AAstrophysicsstrophysics(see also arXiv:0705.0116)(see also arXiv:0705.0116)




SupernovaSupernovaNeutrino OscillationsNeutrino Oscillations


Neutrino Flavor OscillationsNeutrino Flavor Oscillations

Two-flavor mixingTwo-flavor mixing

2

1e

cossin

sincos

2

1e

cossin

sincos

Bruno PontecorvoBruno Pontecorvo(1913 – 1993)(1913 – 1993)

Invented nu oscillationsInvented nu oscillations

Each mass eigenstate propagates asEach mass eigenstate propagates as

with with

ipzeipze

E2m

EmEp2

22 E2

mEmEp

222

zE2

m2z

E2m2

Phase difference implies flavor oscillationsPhase difference implies flavor oscillations

Oscillation Oscillation LengthLength

2

2

2 m

eVMeVE

m5.2m

E4

2

2

2 m

eVMeVE

m5.2m

E4

sinsin22(2(2))

ProbabilityProbability ee

zz


Mixing of Neutrinos with Different MassMixing of Neutrinos with Different Mass

ElectronElectronneutrinoneutrino

NeutrinoNeutrinomass mmass m11

NeutrinoNeutrinomass mmass m22

Neutrino propagation as a wave phenomenonNeutrino propagation as a wave phenomenon

Mass mMass m11

Mass mMass m2 2 = m= m11

Mass mMass m11

Mass mMass m2 2 >> m m11

Mass mMass m11


Mass mMass m11


Mass mMass m11

Mass mMass m22 >> m m11



Neutrino OscillationsNeutrino Oscillations

Mass mMass m11

Mass mMass m22 >> m m11Oscillation lengthOscillation length

21

22 mm

E4

21

22 mm

E4



Neutrino OscillationsNeutrino Oscillations

Oscillation lengthOscillation length

21

22 mm

E4

21

22 mm

E4



Three-Flavor Neutrino ParametersThree-Flavor Neutrino Parameters

3

2

1

1212

1212

1313

1313

2323

2323

e

1

CS

SC

CS

1

SC

CS

SC

1

3

2

1

1212

1212

1313

1313

2323

2323

e

1

CS

SC

CS

1

SC

CS

SC

1 ie ie

ie ie

.,etccosC 1212 .,etccosC 1212 CP-violating phaseCP-violating phase

SolarSolar75759292

AtmosphericAtmospheric1400140030003000

22 meVm 22 meVm

CHOOZCHOOZ Solar/KamLANDSolar/KamLAND 22 ranges rangeshep-ph/0405172hep-ph/0405172

Atmospheric/K2KAtmospheric/K2K 5437 23 5437 23 1113 1113 3630 12 3630 12

ee

ee

11SunSun

NormalNormal

22

33

AtmosphereAtmosphere

ee

ee

11SunSun

InvertedInverted22

33

AtmosphereAtmosphere

Tasks and Open QuestionsTasks and Open Questions

• Precision for Precision for 12 12 andand 2323

• How large is How large is 1313 ??

• CP-violating phase CP-violating phase ??• Mass orderingMass ordering ? ? (normal vs inverted)(normal vs inverted)• Absolute massesAbsolute masses ?? (hierarchical vs degenerate)(hierarchical vs degenerate)• Dirac or MajoranaDirac or Majorana ??


Long-Baseline Experiment K2KLong-Baseline Experiment K2K

K2K ExperimentK2K Experiment(KEK to (KEK to Kamiokande)Kamiokande)has confirmedhas confirmedneutrinoneutrinooscillations,oscillations,to be followedto be followedby T2K (2009)by T2K (2009)


Neutrino Oscillations in MatterNeutrino Oscillations in Matter

• “ “Level crossing” possible in a medium with a gradient (MSW effect)Level crossing” possible in a medium with a gradient (MSW effect) - For solar nus large flavor conversion anyway due to large mixing- For solar nus large flavor conversion anyway due to large mixing - Still important for 13-oscillations in supernova envelope- Still important for 13-oscillations in supernova envelope• Breaks degeneracy between Breaks degeneracy between and and /2 /2 (dark vs light side) (dark vs light side) - 12 mass ordering for solar nus established- 12 mass ordering for solar nus established - 13 mass ordering (normal vs inverted) at future LBL or SN- 13 mass ordering (normal vs inverted) at future LBL or SN• Discriminates against sterile nus in atmospheric oscillationsDiscriminates against sterile nus in atmospheric oscillations• CP asymmetry in LBL, to be distinguished from intrinsic CP violationCP asymmetry in LBL, to be distinguished from intrinsic CP violation• Prevents flavor conversion in a SN core and within shock wavePrevents flavor conversion in a SN core and within shock wave• Strongly affects sterile nu production in SN or early universeStrongly affects sterile nu production in SN or early universe

Lincoln WolfensteinLincoln Wolfenstein

ff

ZZ

W, ZW, Z

ff

Neutrinos in a medium suffer flavor-dependentNeutrinos in a medium suffer flavor-dependentrefraction (PRD 17:2369, 1978)refraction (PRD 17:2369, 1978)

e

n21

n21

eF

2e

n0

0nnG2

E2M

zi

e

n21

n21

eF

2e

n0

0nnG2

E2M

zi

In Earth or Sun weak In Earth or Sun weak potentialpotential

of order 10of order 101313 eV eV


H- and L-Resonance for MSW OscillationsH- and L-Resonance for MSW Oscillations

R. Tomàs, M. Kachelriess,R. Tomàs, M. Kachelriess,G. Raffelt, A. Dighe,G. Raffelt, A. Dighe,H.-T. Janka & L. Scheck: H.-T. Janka & L. Scheck: Neutrino signatures ofNeutrino signatures ofsupernova forward andsupernova forward andreverse shock propagationreverse shock propagation[astro-ph/0407132] [astro-ph/0407132]

ResonancResonanceedensity density forfor

2atmm 2atmm

ResonancResonanceedensity density forfor

2solm 2solm


Shock-Wave Propagation in IceCubeShock-Wave Propagation in IceCube

Choubey, Harries & Ross, “Probing neutrino oscillations from supernovae shockChoubey, Harries & Ross, “Probing neutrino oscillations from supernovae shockwaves via the IceCube detector”, astro-ph/0604300waves via the IceCube detector”, astro-ph/0604300

Normal HierarchyNormal Hierarchy

Inverted HierarchyInverted HierarchyNo shockwaveNo shockwave

Inverted HierarchyInverted HierarchyForward shockForward shock

Inverted HierarchyInverted HierarchyForward & reverse shockForward & reverse shock

,8.0)(Flux)(Flux

x

e

,8.0)(Flux)(Flux

x

e

MeV18E,MeV15Exe

MeV18E,MeV15Exe


Matrices of Density in Flavor SpaceMatrices of Density in Flavor Space

Neutrino quantum fieldNeutrino quantum field

Spinors in flavor spaceSpinors in flavor space

Quantum states (amplitudes)Quantum states (amplitudes)

Variables for discussing neutrino flavor oscillationsVariables for discussing neutrino flavor oscillations

““Matrices of densities” Matrices of densities” (analogous to occupation numbers)(analogous to occupation numbers)

““Quadratic” quantities, required forQuadratic” quantities, required fordealing with decoherence, collisions,dealing with decoherence, collisions,Pauli-blocking, nu-nu-refraction, etc.Pauli-blocking, nu-nu-refraction, etc.

Sufficient for “beam experiments,”Sufficient for “beam experiments,”but confusing “wave packet debates”but confusing “wave packet debates”for quantifying decoherence effectsfor quantifying decoherence effects

xpi

p†

p3

3evp,tbup,ta

2

pd)x,t(

xpi

p†

p3

3evp,tbup,ta

2

pd)x,t(

3

2

1

3

2

1

3

2

1

a

a

a

a

3

2

1

a

a

a

a

3

2

1

b

b

b

b

3

2

1

b

b

b

bDestructionDestructionoperators foroperators for(anti)neutrinos(anti)neutrinos

0

a

p,ta

p,ta

p,t

p,t

p,t†

p,t3

2

1

3

2

1

0

a

p,ta

p,ta

p,t

p,t

p,t†

p,t3

2

1

3

2

1

NeutrinosNeutrinos

Anti-Anti-neutrinosneutrinos

p,tap,tap,t i†jij

p,tap,tap,t i

†jij

p,tbp,tbp,t j†iij

p,tbp,tbp,t j

†iij


General Equations of MotionGeneral Equations of Motion

pqqqp3

3

FpFp

2

pt ),)(cos1(2

qdG2],L[G2,

p2M

i

pqqqp3

3

FpFp

2

pt ),)(cos1(2

qdG2],L[G2,

p2M

i

pqqqp3

3

FpFp

2

pt ),)(cos1(2

qdG2],L[G2,

p2M

i

pqqqp3

3

FpFp

2

pt ),)(cos1(2

qdG2],L[G2,

p2M

i

Usual matter effect withUsual matter effect with

nn00

0nn0

00nn

Lee

nn00

0nn0

00nn

Lee

• Vacuum oscillationsVacuum oscillations M is neutrino mass M is neutrino mass matrixmatrix

• Note opposite sign Note opposite sign betweenbetween neutrinos and neutrinos and antineutrinosantineutrinosNonlinear nu-nu effects are importantNonlinear nu-nu effects are importantwhen nu-nu interaction energy exceedswhen nu-nu interaction energy exceedstypical vacuum oscillation frequencytypical vacuum oscillation frequency(Do not compare with matter effect!)(Do not compare with matter effect!)

cos1nG2E2

mF

2

osc

cos1nG2E2

mF

2

osc


Toy Supernova in “Single-Angle” Toy Supernova in “Single-Angle” ApproximationApproximation

BipolarOscillations

• Assume 80% anti-neutrinosAssume 80% anti-neutrinos• Vacuum oscillation frequencyVacuum oscillation frequency

= 0.3 km= 0.3 km11

• Neutrino-neutrino interaction Neutrino-neutrino interaction energy at nu sphere (r = 10 km)energy at nu sphere (r = 10 km)

= 0.3= 0.3101055 km km11

• Falls off approximately as Falls off approximately as rr44

(geometric flux dilution and nus(geometric flux dilution and nus become more co-linear)become more co-linear)

Decline of oscillation amplitudeDecline of oscillation amplitudeexplained in pendulum analogyexplained in pendulum analogyby inreasing moment of inertiaby inreasing moment of inertia(Hannestad, Raffelt, Sigl & Wong(Hannestad, Raffelt, Sigl & Wong astro-ph/0608695)astro-ph/0608695)


Collective SN neutrino oscillations 2006-2007Collective SN neutrino oscillations 2006-2007

““Bipolar” collective transformationsBipolar” collective transformationsimportant, even for dense matterimportant, even for dense matter

• Duan, Fuller & Qian Duan, Fuller & Qian astro-ph/0511275astro-ph/0511275

Numerical simulationsNumerical simulations• Including multi-angle effectsIncluding multi-angle effects• Discovery of “spectral splits”Discovery of “spectral splits”

• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0606616, 0608050astro-ph/0606616, 0608050

• Pendulum in flavor spacePendulum in flavor space• Collective pair annihilationCollective pair annihilation• Pure precession modePure precession mode

• Hannestad, Raffelt, Sigl & WongHannestad, Raffelt, Sigl & Wong astro-ph/0608695astro-ph/0608695• Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian astro-ph/0703776astro-ph/0703776

Self-maintained coherenceSelf-maintained coherencevs. self-induced decoherencevs. self-induced decoherencecaused by multi-angle effectscaused by multi-angle effects

• Raffelt & Sigl, hep-ph/0701182Raffelt & Sigl, hep-ph/0701182• Esteban-Pretel, Pastor, Tomas,Esteban-Pretel, Pastor, Tomas, Raffelt & Sigl, arXiv:0706.2498Raffelt & Sigl, arXiv:0706.2498

Theory of “spectral splits”Theory of “spectral splits”in terms of adiabatic evolution inin terms of adiabatic evolution inrotating framerotating frame

• Raffelt & Smirnov,Raffelt & Smirnov, arXiv:0705.1830, arXiv:0705.1830, 0709.46410709.4641 • Duan, Fuller, Carlson & QianDuan, Fuller, Carlson & Qian arXiv:0706.4293, 0707.0290 arXiv:0706.4293, 0707.0290

Independent numerical simulationsIndependent numerical simulations • Fogli, Lisi, Marrone & MirizziFogli, Lisi, Marrone & Mirizzi arXiv:0707.1998 arXiv:0707.1998




Cosmic Diffuse Cosmic Diffuse SupernovaSupernova

Neutrino Background Neutrino Background (DSNB)(DSNB)


Diffuse Background Flux of SN NeutrinosDiffuse Background Flux of SN Neutrinos

1 SNu ~ 4 L1 SNu ~ 4 L / L / L,B,B

Average neutrinoAverage neutrinoluminosity of galaxiesluminosity of galaxies~ photon luminosity~ photon luminosity

1 SNu 1 SNu == 1 SN / 10 1 SN / 101010 L Lsun,Bsun,B / 100 years / 100 years

LLsun,Bsun,B == 0.54 L 0.54 Lsunsun == 2 2 10103333 erg/serg/s

EE ~ 3 ~ 3 10105353 erg per core-collapse SN erg per core-collapse SN

For galaxies, averageFor galaxies, averagenuclear & gravitationalnuclear & gravitationalenergy release comparableenergy release comparable

• Photons come from nuclear energyPhotons come from nuclear energy

• Neutrinos from gravitational energyNeutrinos from gravitational energy

Present-day SN rate of ~ 1 SNu, extrapolated to the entire universe,Present-day SN rate of ~ 1 SNu, extrapolated to the entire universe,

corresponds to corresponds to ee flux of ~ 1 cm flux of ~ 1 cm22 s s11

Realistic flux is dominated by much larger early star-formation rateRealistic flux is dominated by much larger early star-formation rate Upper limit ~ 54 cmUpper limit ~ 54 cm22 s s11

[Kaplinghat et al., astro-ph/9912391][Kaplinghat et al., astro-ph/9912391] “ “Realistic estimate” ~ 10 cmRealistic estimate” ~ 10 cm22 s s11

[Hartmann & Woosley, Astropart. Phys. 7 (1997) 137][Hartmann & Woosley, Astropart. Phys. 7 (1997) 137] Measurement would tell us about early history of star formation Measurement would tell us about early history of star formation


Experimental Limits on Relic Supernova Experimental Limits on Relic Supernova NeutrinosNeutrinos

Cline, astro-ph/0103138Cline, astro-ph/0103138

Upper-limit flux ofUpper-limit flux of Kaplinghat et al., Kaplinghat et al., astro-ph/9912391astro-ph/9912391 Integrated 54 cmIntegrated 54 cm-2-2 s s-1-1

Super-K upper limitSuper-K upper limit 29 cm29 cm-2-2 s s-1 -1 for for Kaplinghat et al. Kaplinghat et al. spectrumspectrum [hep-ex/0209028][hep-ex/0209028]


DSNB Measurement with Neutron TaggingDSNB Measurement with Neutron Tagging

Beacom & Vagins, hep-ph/0309300 Beacom & Vagins, hep-ph/0309300 [Phys. Rev. Lett., 93:171101, 2004] [Phys. Rev. Lett., 93:171101, 2004]

Pushing the boundaries of neutrinoPushing the boundaries of neutrinoastronomy to cosmological distancesastronomy to cosmological distances

Future large-scale scintillatorFuture large-scale scintillatordetectors (e.g. LENA with 50 kt)detectors (e.g. LENA with 50 kt)

• Inverse beta decay reaction taggedInverse beta decay reaction tagged• Location with smaller reactor fluxLocation with smaller reactor flux (e.g. Pyh(e.g. Pyhääsalmi in Finland) couldsalmi in Finland) could allow for lower thresholdallow for lower threshold


The Red Supergiant Betelgeuse (Alpha Orionis)The Red Supergiant Betelgeuse (Alpha Orionis)

First resolvedFirst resolvedimage of a starimage of a starother than Sunother than Sun

DistanceDistance(Hipparcos)(Hipparcos)130 pc (425 lyr)130 pc (425 lyr)

If Betelgeuse goes Supernova:If Betelgeuse goes Supernova:• 66 101077 neutrino events in Super-Kamiokande neutrino events in Super-Kamiokande• 2.42.4 101033 neutron events per day from Silicon-burning phase neutron events per day from Silicon-burning phase (few days warning!), need neutron tagging(few days warning!), need neutron tagging [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012] [Odrzywolek, Misiaszek & Kutschera, astro-ph/0311012]


Aachen SkylineAachen Skyline

Looking forward to the next galactic supernova!

georg raffelt, max-planck-institut für physik, münchen physik kolloquium, 19. november 2007, rwth...

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