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Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
III. Supernova NeutrinosIII. Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Sanduleak Sanduleak −−69 20269 202
Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc(160.000 light years)(160.000 light years)
Tarantula NebulaTarantula Nebula
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Sanduleak Sanduleak −−69 20269 202
Large Magellanic Cloud Large Magellanic Cloud Distance 50 kpcDistance 50 kpc(160.000 light years)(160.000 light years)
Tarantula NebulaTarantula Nebula
Supernova 1987ASupernova 1987A23 February 198723 February 1987
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, IndiaGeorg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernovae: Almost as Bright as GalaxiesSupernovae: Almost as Bright as Galaxies
SN 1994D in NGC 4526SN 1994D in NGC 4526SN 1998S in NGC 3877SN 1998S in NGC 3877
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, IndiaGeorg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Mass Transfer in Binary StarsMass Transfer in Binary Stars
Binary system of white dwarfBinary system of white dwarfand evolved companion star,and evolved companion star,beginning to fill the “Roche lobe”beginning to fill the “Roche lobe”
RocheRoche--lobe overflow feeds masslobe overflow feeds massto the compact starto the compact star
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
HeliumHelium--burning starburning star
HeliumHeliumBurningBurning
HydrogenHydrogenBurningBurning
MainMain--sequence starsequence star
Hydrogen BurningHydrogen Burning
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
HeliumHelium--burning starburning star
HeliumHeliumBurningBurning
HydrogenHydrogenBurningBurning
MainMain--sequence starsequence star
Hydrogen BurningHydrogen Burning
Onion structureOnion structure
Degenerate iron core:Degenerate iron core:ρρ ≈≈ 101099 g cmg cm−−33
T T ≈≈ 101010 10 KKMMFeFe ≈≈ 1.5 M1.5 MsunsunRRFeFe ≈≈ 8000 km8000 km
Collapse (implosion)Collapse (implosion)
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Collapse (implosion)Collapse (implosion)ExplosionExplosionNewborn Neutron StarNewborn Neutron Star
~ 50 km~ 50 km
ProtoProto--Neutron StarNeutron Starρρ ≈≈ ρρnucnuc == 33 ××10101414 g cmg cm−−33
T T ≈≈ 30 MeV30 MeV
NeutrinoNeutrinoCoolingCooling
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Newborn Neutron StarNewborn Neutron Star
~ 50 km~ 50 km
ProtoProto--Neutron StarNeutron Starρρ ≈≈ ρρnucnuc == 33 ××10101414 g cmg cm−−33
T T ≈≈ 30 MeV30 MeV
NeutrinoNeutrinoCoolingCooling
Gravitational binding energyGravitational binding energy
EEbb ≈≈ 3 3 ×× 10105353 erg erg ≈≈ 17% M17% 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
LLνν ≈≈ 3 3 ×× 10105353 erg / 3 secerg / 3 sec≈≈ 3 3 ×× 10101919 LLSUNSUN
While it lasts, outshines the entireWhile it lasts, outshines the entirevisible universevisible universe
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrino Signal of Supernova 1987ANeutrino Signal of Supernova 1987A
Within clock uncertainties,Within clock uncertainties,signals are contemporaneoussignals are contemporaneous
KamiokandeKamiokande--II (Japan)II (Japan)Water Cherenkov detectorWater Cherenkov detector2140 tons2140 tonsClock uncertainty Clock uncertainty ±±1 min1 min
IrvineIrvine--MichiganMichigan--Brookhaven (US)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 Clock uncertainty +2/+2/--54 s54 s
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernova Remnant in Cas A (SN 1667Supernova Remnant in Cas A (SN 1667?)?)
Chandra Chandra xx--ray imageray image
Non-pulsarcompact remnant(could be black hole)
Non-pulsarcompact remnant(could be black hole)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
The Crab PulsarThe Crab Pulsar
Chandra x-ray imagesChandra x-ray images
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Baade and Zwicky were the first to speculate about a connectionBaade and Zwicky were the first to speculate about a connectionbetween supernova explosions and neutronbetween supernova explosions and neutron--star formationstar formation
[Phy[Phys. Rev. 45 (1934) 138]s. Rev. 45 (1934) 138]
Walter Baade (1893Walter Baade (1893−−1960)1960) Fritz Zwicky (1898Fritz Zwicky (1898−−1974)1974)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Thermonuclear vs. CoreThermonuclear vs. Core--Collapse SupernovaeCollapse Supernovae
Core collapse (Type II, Ib/c)Core collapse (Type II, Ib/c)Thermonuclear (Type Ia)Thermonuclear (Type Ia)
•• CarbonCarbon--oxygen white dwarfoxygen white dwarf(remnant of(remnant oflowlow--mass star)mass star)
•• Accretes matterAccretes matterfrom companionfrom companion
•• Degenerate iron coreDegenerate iron coreof evolved massive starof evolved massive star
•• Accretes matter Accretes matter by nuclear burningby nuclear burningat its surfaceat its surface
Chandrasekhar limit is reached Chandrasekhar limit is reached −− MMChCh ≈≈ 1.5 M1.5 Msunsun (2Y(2Yee))22
C O L L A P S E S E T S I NC O L L A P S E S E T S I N
Nuclear burning of C and O ignitesNuclear burning of C and O ignites→→ Nuclear deflagrationNuclear deflagration((““Fusion bombFusion bomb”” triggered by collapse)triggered by collapse)
Collapse to nuclear densityCollapse to nuclear densityBounce & shock Bounce & shock Implosion Implosion →→ ExplosionExplosion
Gain of nuclear binding energyGain of nuclear binding energy~ 1 MeV per nucleon ~ 1 MeV per nucleon
Gain of gravitational binding energyGain of gravitational binding energy~~ 100 MeV per nucleon100 MeV per nucleon99% into neutrinos 99% into neutrinos
Powered by gravityPowered by gravityPowered by nuclear binding energyPowered by nuclear binding energy
Comparable Comparable ““visiblevisible”” energy release of energy release of ~ 3 ~ 3 ×× 10105151ergerg
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
No HydrogenNo Hydrogen HydrogenHydrogenSpectrumSpectrum
No SiliconNo SiliconSiliconSilicon
No HydrogenNo Hydrogen HydrogenHydrogenSpectrumSpectrum
Spectral Classification of SupernovaeSpectral Classification of Supernovae
Spectral TypeSpectral Type IbIb IcIc IIIIIaIa
No HeliumNo HeliumHeliumHelium
No SiliconNo SiliconSiliconSilicon
No HydrogenNo Hydrogen HydrogenHydrogen
SpectrumSpectrum
PhysicalPhysicalMechanismMechanism
NuclearNuclearexplosion ofexplosion of
lowlow--mass starmass star
Core collapse of evolved massive starCore collapse of evolved massive star(may have lost its hydrogen or even helium(may have lost its hydrogen or even helium
envelope during redenvelope during red--giant evolution)giant evolution)
Light CurveLight Curve ReproducibleReproducible Large variationsLarge variations
CompactCompactRemnantRemnant NoneNone Neutron star (typically appears as pulsar)Neutron star (typically appears as pulsar)
Sometimes black hole ?Sometimes black hole ?
Rate / hRate / h22 SNuSNu 0.36 0.36 ±± 0.110.11 0.71 0.71 ±± 0.340.340.14 0.14 ±± 0.070.07
ObservedObserved Total Total ∼∼ 2000 as of today (nowadays 2000 as of today (nowadays ∼∼200/year)200/year)
NeutrinosNeutrinos ∼∼ 100 100 ×× Visible energyVisible energyInsignificantInsignificant
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Universal Supernova Ia Light CurveUniversal Supernova Ia Light Curve
Supernova Ia lightcurves areSupernova Ia lightcurves areempirically a 1empirically a 1--parameter familyparameter family
After transformationAfter transformationa universal light curve,a universal light curve,i.e. a dei.e. a de--facto standard candlefacto standard candle
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Examples for SN II Light CurvesExamples for SN II Light Curves
Cappellaro & Turatto,Cappellaro & Turatto,astroastro--ph/0012455ph/0012455
Powered by Powered by radioactive decay of radioactive decay of 5656CoCo
SN 1987ASN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernovae the Power Supply for Cosmic Rays?Supernovae the Power Supply for Cosmic Rays?
Suggestive of supernovae:Suggestive of supernovae:
•• One SN explosion deposits ~ 3 One SN explosion deposits ~ 3 ×× 10105151 erg in kinetic energy oferg in kinetic energy ofejecta into the interstellar medium (ISM)ejecta into the interstellar medium (ISM)
•• Rate approx. 1 SN / 30 years / galaxyRate approx. 1 SN / 30 years / galaxy
Total average energy deposition:Total average energy deposition: LLSNSN ≈≈ 3 3 ×× 10104242 erg/s erg/s ≈≈ 50 50 LLCRCR
Required power supply LRequired power supply LCRCR = V= VDD ρρCRCR//ττresres≈≈ 5 5 ×× 10104040 erg/s erg/s ≈≈ 101077 LLSunSun
Disk volumeDisk volume VVD D = = ππ RR22 d d ≈≈ ππ (15 kpc)(15 kpc)22 200 pc 200 pc ≈≈ 4 4 ×× 10106666 cmcm33
Energy density in CRsEnergy density in CRs ρρCR CR ≈≈ 1 eV / cm1 eV / cm33
Residence time in galaxyResidence time in galaxy ττres res ≈≈ 6 6 ×× 101066 yrsyrs
Efficiency of a few percent requiredEfficiency of a few percent required
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Explosion Mechanismfor Core-Collapse SNeExplosion Mechanismfor Core-Collapse SNe
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Collapse and Prompt ExplosionCollapse and Prompt Explosion
Supernova explosion primarily a hydrodynamical phenomenonSupernova explosion primarily a hydrodynamical phenomenon
Movies by J.A.Font, Numerical Hydrodynamics in General RelativitMovies by J.A.Font, Numerical Hydrodynamics in General Relativityyhttp://www.livingreviews.orghttp://www.livingreviews.org
VelocityVelocity DensityDensity
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Failed ExplosionFailed Explosion
SphericallySpherically symmetricsymmetricsimulation of a 15 Msimulation of a 15 Msunsunstellar model stellar model with statewith state--ofof--thethe--artartneutrino transportneutrino transport
Movie courtesy ofMovie courtesy ofBronson Messer,Bronson Messer,Oakridge group (2001)Oakridge group (2001)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Why No Prompt Explosion?Why No Prompt Explosion?
DissociatedDissociatedMaterialMaterial
(n, p, e, (n, p, e, νν))
•• 0.1 M0.1 Msunsun of iron has a of iron has a nuclear binding energynuclear binding energy≈≈ 1.7 1.7 ×× 10105151 ergerg
•• Comparable toComparable toexplosion energyexplosion energy
•• Shock wave forms Shock wave forms within the iron corewithin the iron core
•• Dissipates its energy Dissipates its energy by dissociating the by dissociating the remaining layer of iron remaining layer of iron
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrinos to the RescueNeutrinos to the Rescue
Picture adapted from Janka, astroPicture adapted from Janka, astro--ph/0008432ph/0008432
Neutrino heatingNeutrino heatingincreases pressureincreases pressurebehind shock frontbehind shock front
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernova Delayed Explosion ScenarioSupernova Delayed Explosion Scenario
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Spherical Symmetry in Astrophysics :-)Spherical Symmetry in Astrophysics :-)
Crab NebulaCrab Nebula
EtaCarinaeEtaCarinae
SN 1987ASN 1987A
Cas ACas A
Crab PulsarCrab
Pulsar
SNR G5.4-1.2PSR 1757-24SNR G5.4-1.2PSR 1757-24
[Adapted after a slide by A.Burrows][Adapted after a slide by A.Burrows]
Convection in SN simulationsConvection in SN simulations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Parametric 2D Studies (180º) by Garching GroupParametric 2D Studies (180º) by Garching Group
•• If explosion developsIf explosion developsslowly, convectiveslowly, convectivestructures have timestructures have timeto merge to lowto merge to low(l = 1 or 2) mode(l = 1 or 2) modeflowflow
•• Very asymmetricVery asymmetricshock expansionshock expansionand mass ejectionand mass ejectionalthough boundaryalthough boundaryneutrino flux is neutrino flux is isotropicisotropic
(Scheck et al., PRL(Scheck et al., PRL2004 and PhD Thesis)2004 and PhD Thesis)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Parametric 3D Studies by Garching GroupParametric 3D Studies by Garching Group
•• First explosions inFirst explosions in3D show also very3D show also verylarge asymmetrylarge asymmetry
•• Convection growsConvection growsfaster than in 2Dfaster than in 2D
•• Explosion energyExplosion energysomewhat highersomewhat higher
(L. Scheck(L. ScheckPhD Thesis 2004)PhD Thesis 2004)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Parametric 3D Studies by Garching GroupParametric 3D Studies by Garching Group
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Convection to the RescueConvection to the Rescue
Picture adapted from Janka, astroPicture adapted from Janka, astro--ph/0008432ph/0008432
Convection dredges energyConvection dredges energyfrom the neutron starfrom the neutron star
to the shock waveto the shock wave
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Exploding Models (8Exploding Models (8--10 Solar Masses) with O10 Solar Masses) with O--NeNe--CoresCores
Kitaura, Janka & Hillebrandt: “Explosions of Kitaura, Janka & Hillebrandt: “Explosions of OO--NeNe--Mg cores, the Crab supernova,Mg cores, the Crab supernova,and subluminous type IIand subluminous type II--P supernovae”, astroP supernovae”, astro--ph/0512065ph/0512065
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
HighHigh--Velocity PulsarsVelocity Pulsars
FalseFalse--color radio image of the SNR G5.4color radio image of the SNR G5.4--1.21.2and the young radio pulsar PSR 1757and the young radio pulsar PSR 1757--24 24 (v = 1300(v = 1300−−1700 km/s away from the gal. plane)1700 km/s away from the gal. plane)
Pulsar velocity distributionPulsar velocity distribution[Lyne & Lorimer, Nature 369 (1994) 127][Lyne & Lorimer, Nature 369 (1994) 127]
Galactic escapeGalactic escapevelocity ~ 600 km/svelocity ~ 600 km/s
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
What Accelerates the Pulsars?What Accelerates the Pulsars?
Hydrodynamically driven kicksHydrodynamically driven kicks•• Asymmetric matter ejection, but is convection enough Asymmetric matter ejection, but is convection enough •• PrePre--collapse asymmetry, perhaps caused by overstable collapse asymmetry, perhaps caused by overstable
oscillations of preoscillations of pre--supernova core? supernova core?
MatterMatterRocketRocket
PhotonPhotonRocketRocket
Electromagnetically driven acceleration:Electromagnetically driven acceleration:OffOff--center global magnetic dipole moment & rotationcenter global magnetic dipole moment & rotationaccelerates star in one direction.accelerates star in one direction.(Slow process (Slow process –– not a “kick”)not a “kick”)
Dong Lai, Neutron Star Kicks and Asymmetric Supernovae, astroDong Lai, Neutron Star Kicks and Asymmetric Supernovae, astro--ph/0012049 ph/0012049
Required neutrino Required neutrino asymmetryasymmetry
Caused by BCaused by B--field induced asymmetry of neutrino transportfield induced asymmetry of neutrino transportcoefficients (parity violation, dispersion effects & oscillatiocoefficients (parity violation, dispersion effects & oscillations,ns,asymmetric field distribution, ...)? asymmetric field distribution, ...)? Typically requires huge fields > 10Typically requires huge fields > 101515 Gauss Gauss
NeutrinoNeutrinoRocketRocket
⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛ ×s/km1000
vE
erg103%8.2 kick
tot
53
⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛ ×s/km1000
vE
erg103%8.2 kick
tot
53
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Gravitational Waves from CoreGravitational Waves from Core--Collapse SupernovaeCollapse Supernovae
MMüüller, Rampp, Buras, Janka, & Shoemaker,ller, Rampp, Buras, Janka, & Shoemaker,“Towards gravitational wave signals from“Towards gravitational wave signals fromrealistic core collapse supernova models,”realistic core collapse supernova models,”astroastro--ph/0309833ph/0309833
The gravitationalThe gravitational--wave signal from convectionwave signal from convectionis a generic and dominating featureis a generic and dominating feature
BounceBounce
ConvectionConvection
Asymmetric neutrino emissionAsymmetric neutrino emission
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Novel Forms of Energy Transfer?Novel Forms of Energy Transfer?
New particles or neutrinos with novel properties could provide aNew particles or neutrinos with novel properties could provide achannel of energy transfer from proto neutron star to shock wavechannel of energy transfer from proto neutron star to shock wave
Must not transfer too much energy: Limits on decaying neutrinosMust not transfer too much energy: Limits on decaying neutrinos[Falk & Schramm, PLB 79 (1978) 511][Falk & Schramm, PLB 79 (1978) 511]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Shock Revival by Novel Particles?Shock Revival by Novel Particles?
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Viable Scenario with AxionViable Scenario with Axion--Like ParticlesLike Particles
Berezhiani & Drago, PLB 473 (2000) 281 Berezhiani & Drago, PLB 473 (2000) 281
Apparently consistent with f Apparently consistent with f == few 10few 1055 GeV and m GeV and m == few MeVfew MeVNot excluded by other arguments, but also not independently motiNot excluded by other arguments, but also not independently motivatedvated
StallingStallingshockshockwavewave
DecayDecay−+ +→ eea −+ +→ eea
PNSPNS Thermal flux of axionThermal flux of axion--likelikeparticles from “axion sphere”particles from “axion sphere”
Coupled to nuclear mediumCoupled to nuclear mediumby bremsstrahlungby bremsstrahlung
aNNNN ++→+ aNNNN ++→+
af1
L e5e µµ ∂ψγγψ= a
f1
L e5e µµ ∂ψγγψ=a
f1
L N5N µµ ∂ψγγψ= a
f1
L N5N µµ ∂ψγγψ=
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Swapping Neutrino Spectra by OscillationsSwapping Neutrino Spectra by Oscillations
StallingStallingshockshockwavewave
Effective energy Effective energy transfertransfer
−+→+ν epne−+→+ν epne++→+ν enpe++→+ν enpe
Not effective Not effective +− +→ν+ν ee +− +→ν+ν ee
PNSPNS
ννeewith with ⟨⟨EE⟩⟩ ≈≈ 12 MeV
12 MeV
ννµµ with with ⟨⟨EE⟩⟩ ≈≈ 20 MeV
20 MeV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Swapping Neutrino Spectra by OscillationsSwapping Neutrino Spectra by Oscillations
Swapping neutrino spectra by flavor oscillations enhances the rSwapping neutrino spectra by flavor oscillations enhances the rate of energyate of energytransfer to stalling shock wave [Fuller et al., ApJ 389 (1992) transfer to stalling shock wave [Fuller et al., ApJ 389 (1992) 517]517]
StallingStallingshockshockwavewave
PNSPNS
νν eewith with
⟨⟨EE⟩⟩ ≈≈ 12 MeV12 MeV
νν µµwith with
⟨⟨EE⟩⟩ ≈≈ 12 MeV12 MeV
ννµµ with with ⟨⟨EE⟩⟩ ≈≈ 20 MeV
20 MeV ννee with with ⟨⟨EE⟩⟩ ≈≈ 20 MeV
20 MeV
FlavorFlavorOscillationsOscillations
Effective energy Effective energy transfertransfer
−+→+ν epne−+→+ν epne++→+ν enpe++→+ν enpe
Not effective Not effective +− +→ν+ν ee +− +→ν+ν ee
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrinos fromCore-Collapse Supernovae
Neutrinos fromCore-Collapse Supernovae
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Structure of Supernova Neutrino SignalStructure of Supernova Neutrino Signal
1.1. Collapse (infall phase)Collapse (infall phase)2.2. Shock break outShock break out3.3. Matter accretionMatter accretion4.4. KelvinKelvin--Helmholtz coolingHelmholtz cooling
Traps Traps neutrinosneutrinosand and leptonleptonnumbernumberof outerof outercore core layerslayers
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutronization Burst as a Standard CandleNeutronization Burst as a Standard Candle
Different MassDifferent Mass Neutrino TransportNeutrino Transport Nuclear EoSNuclear EoS
KachelriessKachelriess,,TomàsTomàs, , BurasBuras,,JankaJanka, , MarekMarek& & RamppRampp,,astroastro--phph/0412082/0412082
If mixingIf mixingscenario isscenario isknown,known,perhaps bestperhaps bestmethod tomethod todeterminedetermineSN distance,SN distance,especially ifespecially ifobscuredobscured
(better than(better than55--10%)10%)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
What determines the size of the PNS?What determines the size of the PNS?
MassMass
Chandrasekhar mass of iron core of progenitor starChandrasekhar mass of iron core of progenitor star
Dimensional analysis:Dimensional analysis:
Same number from zeroSame number from zero--T polytropic modelT polytropic modelsun
2N
3Pl
2N
23NCh M5.1mmmGM ≈=≈ −−−
sun2
N3Pl
2N
23NCh M5.1mmmGM ≈=≈ −−−
DensityDensitySupported by nucleon degeneracy pressureSupported by nucleon degeneracy pressure
Nuclear density Nuclear density 314nuc cmg103 −×=ρ≈ρ 314nuc cmg103 −×=ρ≈ρ
RadiusRadius Ch3
nuc MR3
4=ρ
πCh
3nuc MR
34
=ρπ
km6.10R ≈ km6.10R ≈
SchwarzschildSchwarzschildRadiusRadius
GeneralGeneral
HereHere
MG2R NS = MG2R NS =
km6.4mm2MG2R 2NPlChNS === − km6.4mm2MG2R 2NPlChNS === −
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
What determines the neutrino energies?What determines the neutrino energies?
DegenerateDegenerateCoreCore
PNSPNSAtmosphereAtmosphere
RR
Gravitational potential of a given nucleonGravitational potential of a given nucleon
ΦΦ = = −−GGNNMMPNSPNSmmNN RR−−11
With MWith MPNSPNS ≈≈ 1.5 M1.5 Msunsun and R and R ≈≈ 30 km30 km
ΦΦ ≈≈ −− 27 MeV27 MeV
Virial theorem (hydrostatic equilibrium)Virial theorem (hydrostatic equilibrium)
assuming nondegenerate conditions,assuming nondegenerate conditions,
⟨⟨EEkinkin⟩⟩ = = −− ½ ½ ⟨⟨ΦΦ⟩⟩ ≈≈ 13 MeV13 MeV
Thermal equilibriumThermal equilibrium
T = (2/3) T = (2/3) ⟨⟨EEkinkin⟩⟩ ≈≈ 9 MeV9 MeV
•• If the protoIf the proto--neutron star (PNS) atmosphere is nondegenerate, neutron star (PNS) atmosphere is nondegenerate, its temperature is determined by the gravitational potential its temperature is determined by the gravitational potential at the surfaceat the surfaceof the degenerate core and found in the ~ 10 MeV rangeof the degenerate core and found in the ~ 10 MeV range
•• Core contracts by accretion and/or cooling Core contracts by accretion and/or cooling →→ T increasesT increases
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
What determines the time scale?What determines the time scale?
Main neutrinoMain neutrinoreactionsreactions
Electron flavorElectron flavor
Other flavorsOther flavors
−+→+ν epne−+→+ν epne++→+ν enpe++→+ν enpe
ν+→+ν NNe ν+→+ν NNe
NeutralNeutral--currentcurrentscatteringscatteringcross sectioncross section
224022
F
2A
2V
MeV100E
cm102EGC3C
)NN( ⎟⎟⎠
⎞⎜⎜⎝
⎛×≈
π
+=ν→νσ ν−
ν
224022
F
2A
2V
MeV100E
cm102EGC3C
)NN( ⎟⎟⎠
⎞⎜⎜⎝
⎛×≈
π
+=ν→νσ ν−
ν
Nucleon densityNucleon density 338
N
nucB cm108.1
mn −×≈
ρ= 338
N
nucB cm108.1
mn −×≈
ρ=
Scattering rateScattering rate2
19B MeV100
Es101.1n ⎟⎟
⎠
⎞⎜⎜⎝
⎛×≈σ=Γ ν−
219
B MeV100E
s101.1n ⎟⎟⎠
⎞⎜⎜⎝
⎛×≈σ=Γ ν−
Mean free pathMean free path2
1B E
MeV100cm28)n( ⎟⎟
⎠
⎞⎜⎜⎝
⎛≈σ=λ
ν
−2
1B E
MeV100cm28)n( ⎟⎟
⎠
⎞⎜⎜⎝
⎛≈σ=λ
ν
−
Diffusion timeDiffusion time222
diff MeV100E
km10R
sec2.1R
t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛≈
λ≈ ν
222diff MeV100
Ekm10R
sec2.1R
t ⎟⎟⎠
⎞⎜⎜⎝
⎛⎟⎟⎠
⎞⎜⎜⎝
⎛≈
λ≈ ν
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Convection in Proto Neutron StarConvection in Proto Neutron Star
Keil,Keil, JankaJanka && Müller,Müller, ApJApJ 473473 (1996)(1996) L111L111
Time scale of deleptonization increased Time scale of deleptonization increased by ~ factor 2, i.e. same generalby ~ factor 2, i.e. same generalmagnitude as diffusive transportmagnitude as diffusive transport
Driving Driving ConvectionConvection
Convects by Convects by overshootingovershooting
StableStable
LeptonLepton--rich region
rich region
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
FlavorFlavor--Dependent Fluxes and SpectraDependent Fluxes and Spectra
Broad characteristicsBroad characteristics•• Duration a few secondsDuration a few seconds•• ⟨⟨EEνν⟩⟩ ~ ~ 1010−−20 MeV20 MeV•• ⟨⟨EEνν⟩⟩ increases with timeincreases with time•• Hierarchy of energiesHierarchy of energies
•• Approximate equipartitionApproximate equipartitionof energy between flavorsof energy between flavors
xee EEE ννν << xee EEE ννν <<
Livermore numerical modelLivermore numerical modelApJ 496 (1998) 216ApJ 496 (1998) 216
Prompt Prompt ννeedeleptonizationdeleptonizationburstburst
ννee
ννee
ννxx__
However, in traditionalHowever, in traditionalsimulations transport simulations transport of of ννµµ and and ννττ schematicschematic
•• Incomplete microphysicsIncomplete microphysics
•• Crude numerics to coupleCrude numerics to coupleneutrino transport withneutrino transport withhydro codehydro code
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Literature Scan of FlavorLiterature Scan of Flavor--Dependent Neutrino SpectraDependent Neutrino Spectra
Keil, Janka & Raffelt, astroKeil, Janka & Raffelt, astro--ph/0208035ph/0208035
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernova Neutrino Spectra FormationSupernova Neutrino Spectra Formation
Electron flavorElectron flavor (( ))ee,νν ee,νν
Free Free streamingstreaming−↔ν epne
−↔ν epne
+↔ν enpe+↔ν enpe
Thermal Equilibrium
Neutrino sphere (TNeutrino sphere (TNSNS))
Other flavorsOther flavors (( ))τµτµ νννν ,,, τµτµ νννν ,,,
DiffusionDiffusionThermal Equilibrium
Scattering AtmosphereScattering Atmosphere
ν↔ν NN ν↔ν NN
ν↔ν NN ν↔ν NN
νν↔ NNNN νν↔ NNNNνν↔−+ee νν↔−+ee
ee ν↔ν ee ν↔ν
Free Free streamingstreaming
µνµν↔νν ee µνµν↔νν ee
Transport sphereTransport sphereEnergy sphere (TEnergy sphere (TESES))
Raffelt (astroRaffelt (astro--ph/0105250), Keil, Raffelt & Janka (astroph/0105250), Keil, Raffelt & Janka (astro--ph/0208035)ph/0208035)
TTfluxflux~~ TTNSNS
TTfluxflux~0.6T~0.6TESES
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
FlavorFlavor--Dependent Neutrino Fluxes vs. Equation of StateDependent Neutrino Fluxes vs. Equation of State
Kitaura, Janka & Hillebrandt, “Explosions of OKitaura, Janka & Hillebrandt, “Explosions of O--NeNe--Mg cores, the CrabMg cores, the Crabsupernova, and subluminous Type IIsupernova, and subluminous Type II--P supernovae”, astroP supernovae”, astro--ph/0512065ph/0512065
Wolff & Hillebrandt nuclear EoS (stiff)
eνeν
τµτµ νν ,, ,
Lattimer & Swesty nuclear EoS (soft)
eνeν
τµτµ νν ,, ,
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Microphysics for MuMicrophysics for Mu-- and Tauand Tau--Neutrino TransportNeutrino Transport
[1] Suzuki, Num. Astrophys. Japan 2 (1991) 267[1] Suzuki, Num. Astrophys. Japan 2 (1991) 267[2] Janka, W.Keil, Raffelt & Seckel, PRL 76 (1996) 2621 [astro[2] Janka, W.Keil, Raffelt & Seckel, PRL 76 (1996) 2621 [astro--ph/9507023]ph/9507023][3] Hannestad & Raffelt, ApJ 507 (1998) 339 [astro[3] Hannestad & Raffelt, ApJ 507 (1998) 339 [astro--ph/9711132]ph/9711132][4] Thompson, Burrows & Horvath, PRC 62 (2000) 035802 [astro[4] Thompson, Burrows & Horvath, PRC 62 (2000) 035802 [astro--ph/0003054]ph/0003054][6] Raffelt, ApJ 561 (2001) 890 [astro[6] Raffelt, ApJ 561 (2001) 890 [astro--ph/0105250] ph/0105250] [6] Buras, Janka, M.Keil, Raffelt & Rampp, ApJ (2003) [astro[6] Buras, Janka, M.Keil, Raffelt & Rampp, ApJ (2003) [astro--ph/0205006]ph/0205006][7] M.Keil, Raffelt & Janka, ApJ (2003) [astro[7] M.Keil, Raffelt & Janka, ApJ (2003) [astro--ph/0208035] ph/0208035]
Main opacityMain opacity
Energy exchangeEnergy exchange
Pair productionPair production
Traditional treatmentTraditional treatment Dominant processesDominant processes
N Nν + → + νN Nν + → + ν N Nν + → + νN Nν + → + ν
e eν + → + νe eν + → + νe eν + → + νe eν + → + ν
RecoilRecoil N Nν + → + νN Nν + → + ν
e e+ −+ → ν + νe e+ −+ → ν + νN N N N+ → + + ν + νN N N N+ → + + ν + ν
e eν + ν → ν + νe eν + ν → ν + ν
[2,6,7][2,6,7]
[1[1-- 4]4]
[6,7][6,7]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Flux and Spectra Modification by New ProcessesFlux and Spectra Modification by New Processes
Keil, Raffelt & Janka, ApJ (2003) [astroKeil, Raffelt & Janka, ApJ (2003) [astro--ph/0208035]ph/0208035]
TraditionalTraditional
+ Bremsstrahlung+ Bremsstrahlung
TraditionalTraditional
νν→ NNNN νν→ NNNN+ Bremsstrahlung+ Bremsstrahlung
TraditionalTraditional
+ Nucleon recoil+ Nucleon recoilν→ν NN ν→ν NN
νν→ NNNN νν→ NNNN+ Bremsstrahlung+ Bremsstrahlung
TraditionalTraditional
+ Neutrino pair+ Neutrino pair
+ Nucleon recoil+ Nucleon recoilν→ν NN ν→ν NN
νν→ NNNN νν→ NNNN
µµνν→νν ee µµνν→νν ee
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
What Are The Spectral Flux CharacteristicsWhat Are The Spectral Flux Characteristics??
TwoTwo--parameterparameterfitsfits(Normalization(Normalization isisthirdthird parameter)parameter)
Thermal spectrum,Thermal spectrum,i.e. Fermii.e. Fermi--Dirac shapeDirac shape((ηη fit)fit)
Quasi power lawQuasi power law((αα fit)fit)
The spectra are crudely thermal,The spectra are crudely thermal,but how to characterize in detail?but how to characterize in detail?
Commonly used global parametersCommonly used global parameters
•• Total luminosity Total luminosity LLνν•• Average energyAverage energy ⟨⟨EE⟩⟩•• General energy moments General energy moments ⟨⟨EEnn⟩⟩
•• “RMS energy”“RMS energy”
eνeν
eνeν
ττµµ νννν ,,, ττµµ νννν ,,,
E
EE
3
rms =E
EE
3
rms =
TE
2
e1
E)E(F +η−+
∝ TE
2
e1
E)E(F +η−+
∝
⎥⎦⎤
⎢⎣⎡ +α−∝ α
EE
)1(expE)E(F ⎥⎦⎤
⎢⎣⎡ +α−∝ α
EE
)1(expE)E(F
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Alpha vs. Eta FitAlpha vs. Eta Fit
Starting with the width is reduStarting with the width is reduced in 10% stepsced in 10% steps⎟⎠⎞
⎜⎝⎛ −∝
EE
3expE)E(F 2 ⎟⎠⎞
⎜⎝⎛ −∝
EE
3expE)E(F 2
TE
2
e1
E)E(F +η−+
∝ TE
2
e1
E)E(F +η−+
∝⎥⎦⎤
⎢⎣⎡ +α−∝ α
EE
)1(expE)E(F ⎥⎦⎤
⎢⎣⎡ +α−∝ α
EE
)1(expE)E(F
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Supernova 1987ASupernova 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
SN 1987A Rings (Hubble Space Telescope 4/1994)SN 1987A Rings (Hubble Space Telescope 4/1994)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
SN 1987A Rings (Hubble Space Telescope 4/1994)SN 1987A Rings (Hubble Space Telescope 4/1994)
Supernova Remnant Supernova Remnant (SNR) 1987A (SNR) 1987A
Foreground StarForeground Star
Foreground StarForeground Star
500 Light-days500 Light-days
Ring system consists of Ring system consists of material ejected frommaterial ejected fromthe progenitor star,the progenitor star,illuminated by UV flash illuminated by UV flash from SN 1987Afrom SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Distance Determination with Inner RingDistance Determination with Inner Ring
500
light
500
light
--day
sda
ys ∆∆tt11 ≈≈ 80 days80 days
∆∆tt22 ≈≈ 380 days380 days
≈≈ 50 kpc50 kpc ≈≈ 170,000 light170,000 light--yearsyears
ΘΘ = (1.242 = (1.242 ±± 0.022)0.022)””
Angular diameter Angular diameter ΘΘ++ = (1.716 = (1.716 ±± 0.022)0.022)””measured by HST on 24measured by HST on 24--88--19901990
∆∆tt11 and and ∆∆tt22 measured measured in UV by IUE satellite in UV by IUE satellite
Ni III] light curve SN 1987A ring, measured by IUENi III] light curve SN 1987A ring, measured by IUE[Sonneborn et al. ApJ 477 (1997) 848,[Sonneborn et al. ApJ 477 (1997) 848,fit by fit by Gould & Uza, ApJ 494 (1998) 118]Gould & Uza, ApJ 494 (1998) 118]
Distance to SN 1987ADistance to SN 1987A
51.2 ± 3.1 kpc Panagia et al., 51.2 ± 3.1 kpc Panagia et al., ApJ 380 (1991) L23 ApJ 380 (1991) L23
51.4 ± 1.2 kpc Panagia, 51.4 ± 1.2 kpc Panagia, IAU Symposium 190 (1999)IAU Symposium 190 (1999)
47.2 ± 0.9 kpc Gould & Uza, 47.2 ± 0.9 kpc Gould & Uza, ApJ 494 (1998) 118ApJ 494 (1998) 118
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
SN 1987A SN 1987A -- Explosion Hits Inner RingExplosion Hits Inner Ring
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrino Signal of SN 1987A in KamiokandeNeutrino Signal of SN 1987A in Kamiokande
SN 1987ASN 1987A
Background NoiseBackground Noise
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrino Signal of Supernova 1987ANeutrino Signal of Supernova 1987A
Within clock uncertainties,Within clock uncertainties,signals are contemporaneoussignals are contemporaneous
KamiokandeKamiokande--II (Japan)II (Japan)Water Cherenkov detectorWater Cherenkov detector2140 tons2140 tonsClock uncertainty Clock uncertainty ±±1 min1 min
IrvineIrvine--MichiganMichigan--Brookhaven (US)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 Clock uncertainty +2/+2/--54 s54 s
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
SN 1987A Event No.9 in Kamiokande SN 1987A Event No.9 in Kamiokande
Kamiokande DetectorKamiokande Detector
Hirata et al., PRD 38 (1988) 448Hirata et al., PRD 38 (1988) 448
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
SN 1987A Signal in LSD (Mont Blanc)SN 1987A Signal in LSD (Mont Blanc) ??
LSD (Liquid Scintillator Detector)LSD (Liquid Scintillator Detector)in the Mont Blanc Tunnelin the Mont Blanc Tunnel(Oct. 1984 (Oct. 1984 -- March 1999)March 1999)Supernova monitor for our galaxySupernova monitor for our galaxy90 tons scintillator90 tons scintillator
200 tons iron (support structure)200 tons iron (support structure)
•• Observed a 5Observed a 5--event clusterevent cluster4.72 hours before IMB/Kam4.72 hours before IMB/Kam--IIII
•• Triggered autmatic SN alertTriggered autmatic SN alert•• Statistical fluctuation very unlikelyStatistical fluctuation very unlikely•• No significant signal in IMB/KamNo significant signal in IMB/Kam--IIII
at LSD timeat LSD time•• No significant LSD signal at IMB timeNo significant LSD signal at IMB time
•• Interpretation as “double bang”:Interpretation as “double bang”:Huge Huge ννee flux (~ 40 MeV) at LSD timeflux (~ 40 MeV) at LSD time
•• LSD signal caused by interactionsLSD signal caused by interactionsin iron of support structurein iron of support structure
•• Second bang ordinary multiSecond bang ordinary multi--flavorflavorsignalsignal
(Imshennik & Ryazhskaya,(Imshennik & Ryazhskaya,“A rotating collapsar and possible“A rotating collapsar and possibleinterpretation of the LSD neutrinointerpretation of the LSD neutrinosignal from SN 1987A”, signal from SN 1987A”, astroastro--ph/0401613) ph/0401613)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Early Lightcurve of SN 1987AEarly Lightcurve of SN 1987A
Adapted fromAdapted fromArnett et al.,Arnett et al.,ARAA 27 (1989)ARAA 27 (1989)
ExpectedExpectedvisual visual brightnessbrightnessevolutionevolution
ExpectedExpectedbolometric bolometric brightnessbrightnessevolutionevolution
Neutrinos severalNeutrinos severalhours before light hours before light
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Dispersion between Neutrinos and PhotonsDispersion between Neutrinos and Photons
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 withinSN 1987A: Transit time for photons and neutrinos equal to within ~ 3h~ 3h
Equal within ~ 1 Equal within ~ 1 −− 4 4 ××1010−−33
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 Proves directly that neutrinos respond to gravity in the usual waywaybecause for photons gravitational lensing already proves thisbecause for photons gravitational lensing already proves this pointpoint
•• Cosmological limits Cosmological limits ∆∆NNνν ≲≲ 1 much worse test of neutrino gravitation,1 much worse test of neutrino gravitation,i.e. SN 1987A proves that neutrinos in cosmology gravitate asi.e. SN 1987A proves that neutrinos in cosmology gravitate as they shouldthey should
•• Provides limits on parameters of certain nonProvides limits on parameters of certain non--GR theories of gravitationGR theories of gravitation•• Photons likely obscured for next galactic SN, so this result prPhotons likely obscured for next galactic SN, so this result probablyobably
unique to SN 1987A unique to SN 1987A
∫ months51dt)]t(r[U2t BAShapiro −≈−=∆ ∫ months51dt)]t(r[U2t BAShapiro −≈−=∆
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Neutrino Cross Section in a Water TargetNeutrino Cross Section in a Water Target
Main reactions: dominates for Main reactions: dominates for SNSN
dominadominates for Suntes for Sun
CrossCrosssectionsection
perperwaterwater
moleculemolecule
++→+ν enpe++→+ν enpe
−+→+ν eFO 1616e
−+→+ν eFO 1616e
ν+→+ν −− ee ν+→+ν −− ee
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Angular Distribution of SN 1987A NeutrinosAngular Distribution of SN 1987A Neutrinos
Main detection reactionMain detection reaction
is essentially isotropic for theis essentially isotropic for therelevant energies.relevant energies.
Expect only a fraction of anExpect only a fraction of anevent from forwardevent from forward--peakedpeakedreactionreaction
++→+ν enpe++→+ν enpe
ν+→+ν −− ee ν+→+ν −− ee
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Trigger Efficiencies at the Detectors Trigger Efficiencies at the Detectors
Fiducial volumes for Fiducial volumes for SN 1987A detectionSN 1987A detection
Kamiokande IIKamiokande II2140 tons water2140 tons water(1.43(1.43××10103232 protons)protons)
IMBIMB6800 tons water6800 tons water(4.6(4.6××10103232 protons)protons)
BSTBST200 tons scintillator200 tons scintillator(1.88(1.88××10103131 protons)protons)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Energy Distribution of SN 1987A NeutrinosEnergy Distribution of SN 1987A Neutrinos
Kamiokande IIKamiokande II
IMBIMB
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Interpreting SN 1987A NeutrinosInterpreting SN 1987A Neutrinos
Tota
l Bin
ding
Ene
rgy
Tota
l Bin
ding
Ene
rgy
95 % CLContours
Jegerlehner, Jegerlehner, Neubig & Raffelt,Neubig & Raffelt,PRD 54 (1996) 1194PRD 54 (1996) 1194
Assume thermalAssume thermalspectra andspectra andequipartition ofequipartition ofenergy between energy between the six degrees the six degrees of freedom of freedom ννee,, ννµµ,, ννττ and theirand theirantiparticlesantiparticlesSpectral Spectral ννee TemperatureTemperature
__
TheoryTheory
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany JIGSAW 07, 12-23 Feb 2007, TIFR, Mumbai, India
Cooling Time ScaleCooling Time Scale
Exponential coolingExponential coolingmodelmodelT = TT = T00 ee−−t/4t/4ττ
constant radiusconstant radiusL = LL = L00 ee−−t/t/ττ
Fit parameters areFit parameters areTT00, , ττ, radius,, radius,3 offset times3 offset timesfor detectorsfor detectors
(Loredo & Lamb,(Loredo & Lamb,astroastro--ph/0107260)ph/0107260)
Similar results forSimilar results formore sophisticatedmore sophisticatedcooling modelscooling models
95% CL95% CLcontourcontour