Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrinos and the starsNeutrinos and the starsSupernova NeutrinosSupernova Neutrinos
Georg Raffelt, MPI for PhysicsLectures at the Topical SeminarNeutrino Physics & Astrophysics1721 Sept 2008, Beijing, China
Georg Raffelt, MPI for PhysicsLectures at the Topical SeminarNeutrino Physics & Astrophysics1721 Sept 2008, Beijing, China
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Crab NebulaCrab Nebula
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Stellar Collapse and Supernova ExplosionStellar Collapse and Supernova Explosion
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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 Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Thermonuclear vs. Core-Collapse SupernovaeThermonuclear vs. Core-Collapse Supernovae
Core collapse (Type II, Ib/c)Core collapse (Type II, Ib/c)Thermonuclear (Type Ia)Thermonuclear (Type Ia)
Chandrasekhar limit is reached Chandrasekhar limit is reached M MChCh 1.5 M 1.5 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 bomb” triggered by collapse)(“Fusion bomb” triggered by collapse)
Collapse to nuclear densityCollapse to nuclear density Bounce & shock Bounce & shock Implosion Implosion Explosion Explosion
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 nucleon~ 100 MeV per nucleon 99% into neutrinos 99% into neutrinos
Powered by gravityPowered by gravityPowered by nuclear binding energyPowered by nuclear binding energy
Comparable “visible” energy release of ~ 3 Comparable “visible” energy release of ~ 3 10 105151ergerg
• Carbon-oxygen white dwarfCarbon-oxygen white dwarf (remnant of(remnant of low-mass star)low-mass star)• Accretes matterAccretes matter from companionfrom companion
• Degenerate iron coreDegenerate iron core of evolved massive starof evolved massive star• Accretes matter Accretes matter by nuclear burningby nuclear burning at its surfaceat its surface
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Explosion Mechanismfor Core-Collapse SNeExplosion Mechanismfor Core-Collapse SNe
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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 RelativityMovies by J.A.Font, Numerical Hydrodynamics in General Relativityhttp://www.livingreviews.orghttp://www.livingreviews.org
VelocityVelocity DensityDensity
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Why No Prompt Explosion?Why No Prompt Explosion?
DissociatedDissociatedMaterialMaterial
(n, p, e, (n, p, e, ))
• 0.1 M0.1 Msunsun of iron has a of iron has a
nuclear binding energynuclear binding energy 1.7 1.7 10 105151 erg erg• Comparable toComparable to explosion 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 Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrinos to the RescueNeutrinos to the Rescue
Picture adapted from Janka, astro-ph/0008432Picture adapted from Janka, astro-ph/0008432
Neutrino heatingNeutrino heatingincreases pressureincreases pressurebehind shock frontbehind shock front
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Delayed Explosion ScenarioSupernova Delayed Explosion Scenario
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Gravitational Waves from Core-Collapse Gravitational Waves from Core-Collapse SupernovaeSupernovae
MMüüller, Rampp, Buras, Janka, & Shoemaker,ller, Rampp, Buras, Janka, & Shoemaker, “ “Towards gravitational wave signals fromTowards gravitational wave signals from realistic core collapse supernova models,”realistic core collapse supernova models,” astro-ph/0309833astro-ph/0309833
The gravitational-wave signal from convectionThe gravitational-wave 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 Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987ASome Particle-Physics
Lessons from SN 1987A
Some Particle-PhysicsLessons from SN
1987A
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrino Mass Sensitivity by Signal DispersionNeutrino Mass Sensitivity by Signal Dispersion
Time-of-flight delayTime-of-flight delay of massive neutrinosof massive neutrinos
22
eV1m
EMeV10
kpc10D
ms1.5t
22
eV1m
EMeV10
kpc10D
ms1.5t
SN 1987ASN 1987A (50 kpc)(50 kpc) mm
≲≲ 20 eV 20 eV E E 20 MeV, 20 MeV, t t 10 s 10 s Simple estimate or detailed maximumSimple estimate or detailed maximum likelihood analysis give similar resultslikelihood analysis give similar results
Future Future Galactic SNGalactic SN at 10 kpcat 10 kpc (Super-K)(Super-K)
mm ~ 3 eV~ 3 eV
Rise-time of signal ~ 10 msRise-time of signal ~ 10 ms(Totani, PRL 80:2040, 1998)(Totani, PRL 80:2040, 1998)
mm ~ 1 eV~ 1 eV
Full signalFull signal(Nardi & Zuluaga, (Nardi & Zuluaga, NPB 731:140, 2005)NPB 731:140, 2005)
With lateWith late black-holeblack-hole formationformation
mm ~ 2 eV~ 2 eV
Cutoff “infinitely” fastCutoff “infinitely” fast (Beacom et al., PRD 63:073011, 2001)(Beacom et al., PRD 63:073011, 2001)
mm ~ 1~ 12 eV2 eV
D D 750 kpc, 750 kpc, t t 10 s 10 s few tens of eventsfew tens of events
Future SN inFuture SN in AndromedaAndromeda (Megatonne)(Megatonne)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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 brightnesbrightnesssevolutionevolution
ExpectedExpectedbolometribolometric c brightnesbrightnesssevolutionevolution
Neutrinos severalNeutrinos severalhours before hours before light light
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
DirectDirectsearchsearch
Too muchToo muchcold dark mattercold dark matter
TeleTelescopescopeExperimentsExperiments
Globular clustersGlobular clusters(a-(a--coupling)-coupling)
Too manyToo manyeventsevents
Too muchToo muchenergy lossenergy loss
SN 1987A (a-N-coupling)SN 1987A (a-N-coupling)
Axion BoundsAxion Bounds
101033 101066 101099 10101212 [GeV] f[GeV] faa
eVeVkeVkeV meVmeV eVeVmmaa
Too much hot dark matterToo much hot dark matter
CASTCAST ADMXADMX
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Sterile NeutrinosSterile Neutrinos
To avoid complete energy loss in ~ 1 sTo avoid complete energy loss in ~ 1 s
sinsin22(2(2eses) ) ≲≲ 3 3 10 101010
Average scattering rate in SN coreAverage scattering rate in SN coreinvolving ordinary left-handed neutrinosinvolving ordinary left-handed neutrinos
110L s10 110L s10
Electron neutrino appears as sterile neutrinoElectron neutrino appears as sterile neutrino
in ½ sinin ½ sin22(2(2eses) of all cases) of all cases
Les2
21
s )2(sin Les2
21
s )2(sin
1110es
221 s1s10)2(sin 1110
es2
21 s1s10)2(sin
Active-sterileActive-sterilemixingmixing
ssee
ppWW
nn
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Sterile Neutrino LimitsSterile Neutrino Limits
See also:See also:
Maalampi & Peltoniemi:Maalampi & Peltoniemi: Effects of the 17-keVEffects of the 17-keV neutrino in supernovae neutrino in supernovae PLB 269:357,1991PLB 269:357,1991 Hidaka & Fuller:Hidaka & Fuller: Dark matter sterileDark matter sterile neutrinos in stellarneutrinos in stellar collapse: alteration ofcollapse: alteration of energy/lepton numberenergy/lepton number transport and atransport and a mechanism formechanism for supernova explosionsupernova explosion enhancementenhancement PRD 74:125015,2006 PRD 74:125015,2006
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova 1987A Limit on Large Extra Supernova 1987A Limit on Large Extra DimensionsDimensions
Cullen & Perelstein, hep-ph/9904422Cullen & Perelstein, hep-ph/9904422 Hanhart et al., nucl-th/0007016Hanhart et al., nucl-th/0007016
SN 1987A energy-loss argument:SN 1987A energy-loss argument:
R R 1 1 mmm, M m, M 9 TeV 9 TeV (n (n = = 2)2)
R R 1 nm, M 1 nm, M 0.7 TeV (n 0.7 TeV (n == 3) 3)
Originally the most restrictiveOriginally the most restrictive limit on such theories, exceptlimit on such theories, except for cosmological argumentsfor cosmological arguments
SN core emits large flux of SN core emits large flux of KK gravity modes byKK gravity modes bynucleon-nucleon bremsstrahlungnucleon-nucleon bremsstrahlung
Large multiplicity of modesLarge multiplicity of modes
RT ~ 10RT ~ 101111
for R ~ 1 mm, T ~ 30 MeVfor R ~ 1 mm, T ~ 30 MeV
2PlMRate 2PlMRate
n2Pl
n
2Pl
n
M
T
M
)RT(Rate n2
Pl
n
2Pl
n
M
T
M
)RT(Rate
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987ANeutrinos from the
Next Galactic Supernova
Neutrinos from theNext Galactic
Supernova
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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.
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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,1923A, 1945B,1945B, 1950B,1950B, 1957D,1957D, 1968L,1968L,1983N 1983N
NGC 6946 NGC 6946 D = (5.5 ± 1) MpcD = (5.5 ± 1) Mpc
Observed Supernovae:Observed Supernovae:1917A,1917A, 1939C,1939C, 1948B,1948B, 1968D,1968D, 1969P,1969P,1980K,1980K, 2002hh,2002hh, 2004et,2004et, 2008S2008S
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Pointing with NeutrinosSupernova Pointing with Neutrinos
• Beacom & Vogel: Can a supernova be located by its neutrinos?Beacom & Vogel: Can a supernova be located by its neutrinos? [astro-ph/9811350] [astro-ph/9811350] • Tomàs, Semikoz, Raffelt, Kachelriess & Dighe: Supernova pointing withTomàs, Semikoz, Raffelt, Kachelriess & Dighe: Supernova pointing with low- and high-energy neutrino detectors [hep-ph/0307050]low- and high-energy neutrino detectors [hep-ph/0307050]
ee ee
nepe nepe
SKSK
SK SK 30 30
Neutron tagging efficiencyNeutron tagging efficiency
90 90 %%NoneNone
7.8º7.8º 3.2º3.2º
1.4º1.4º 0.6º0.6º
9595%% CL half-cone opening angle CL half-cone opening angle
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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 < 500 Hz< 500 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 byHalzen, Jacobsen & ZasHalzen, Jacobsen & Zasastro-ph/9512080astro-ph/9512080
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
LAGUNA - Approved FP7 Design StudyLAGUNA - Approved 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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Neutrinos FromAll Cosmic Supernovae
Neutrinos FromAll Cosmic Supernovae
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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]
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Oscillations of Supernova Neutrinos
Oscillations of Supernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Structure of Supernova Neutrino SignalStructure of Supernova Neutrino Signal
1. Collapse (infall phase)1. Collapse (infall phase)2. Shock break out2. Shock break out3. Matter accretion3. Matter accretion4. Kelvin-Helmholtz cooling4. Kelvin-Helmholtz cooling
Traps Traps neutrinosneutrinosand and leptonleptonnumbernumberof outerof outercore core layerslayers
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutronization Burst as a Standard CandleNeutronization Burst as a Standard Candle
Different MassDifferent Mass Neutrino TransportNeutrino Transport Nuclear EoSNuclear EoS
Kachelriess,Kachelriess,Tomàs, Buras,Tomàs, Buras,Janka, MarekJanka, Marek& Rampp,& Rampp,astro-phastro-ph/0412082/0412082
If mixingIf mixingscenario isscenario isknown,known,perhaps bestperhaps bestmethod tomethod todeterminedetermineSN distance,SN distance,especially ifespecially ifobscuredobscured
(better than(better than 5-10%)5-10%)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Flavor-Dependent Fluxes and SpectraFlavor-Dependent Fluxes and Spectra
Broad characteristicsBroad characteristics• Duration a few secondsDuration a few seconds
• EE ~ ~ 101020 MeV20 MeV
• EE increases with timeincreases with time
• Hierarchy of energiesHierarchy of energies
• Approximate equipartitionApproximate equipartition
of energy between flavorsof energy between flavors
xeeEEE xeeEEE
Livermore numerical modelLivermore numerical modelApJ 496 (1998) 216ApJ 496 (1998) 216
Prompt Prompt ee
deleptonizationdeleptonizationburstburst
ee
ee
xx__ However, in traditionalHowever, in traditional
simulations transport simulations transport
of of and and schematic schematic
• Incomplete microphysicsIncomplete microphysics
• Crude numerics to coupleCrude numerics to couple neutrino transport withneutrino transport with hydro codehydro code
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Flavor-Dependent Neutrino Fluxes vs. Equation Flavor-Dependent Neutrino Fluxes vs. Equation of Stateof State
Kitaura, Janka & Hillebrandt, “Explosions of O-Ne-Mg cores, the CrabKitaura, Janka & Hillebrandt, “Explosions of O-Ne-Mg cores, the Crabsupernova, and subluminous Type II-P supernovae”, astro-ph/0512065supernova, and subluminous Type II-P supernovae”, astro-ph/0512065
Wolff & Hillebrandt nuclear EoS (stiff)Lattimer & Swesty nuclear EoS (soft)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Level-Crossing Diagram in a SN EnvelopeLevel-Crossing Diagram in a SN Envelope
Dighe & Smirnov, Identifying the neutrino mass spectrum from a supernovaDighe & Smirnov, Identifying the neutrino mass spectrum from a supernovaneutrino burst, astro-ph/9907423neutrino burst, astro-ph/9907423
Normal mass hierarchyNormal mass hierarchy Inverted mass hierarchyInverted mass hierarchy
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Spectra Emerging from SupernovaeSpectra Emerging from Supernovae
Primary fluxesPrimary fluxes
for for
for for
for for
0eF0eF0eF0eF0xF0xF
ee
ee
,,, ,,,
After leaving theAfter leaving the supernova envelope,supernova envelope, the fluxes arethe fluxes are partially swappedpartially swapped
0x
0e
0e F)p1(FpF 0
x0e
0e F)p1(FpF
0x
0e
0e F)p1(FpF 0
x0e
0e F)p1(FpF
0e
0e
0xx4
1 F4p1
F4p1
F4
pp2F
0
e0e
0xx4
1 F4p1
F4p1
F4
pp2F
NormalNormal
InvertedInverted
sinsin22(2(21313))
≲≲ 101055
≳≳ 101033
AnyAny
Mass orderingMass ordering
sinsin22((1212)) 0.30.3
00 coscos22((1212)) 0.70.7
sinsin22((1212)) 0.30.3coscos22((1212)) 0.70.7
00
CaseCase
AA
BB
CC
Survival probabilitySurvival probability
)for(p e )for(p e )for(p e )for(p e
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Oscillation of Supernova Anti-NeutrinosOscillation of Supernova Anti-Neutrinos
Measured Measured spectrum at a detector like spectrum at a detector like Super-Kamiokande Super-Kamiokande
ee Assumed flux parametersAssumed flux parameters
Flux ratioFlux ratio 1:8.0:e 1:8.0:e
MeV15)(E e MeV15)(E e
MeV18)(E x MeV18)(E x
Mixing parametersMixing parameters
22sun meV60m 22sun meV60m
9.0)2(sin2 9.0)2(sin2
(Dighe, Kachelriess, Keil, Raffelt, Semikoz, Tomàs),(Dighe, Kachelriess, Keil, Raffelt, Semikoz, Tomàs), hep-ph/0303210, hep-ph/0304150, hep-ph/0307050, hep-ph/0311172 hep-ph/0303210, hep-ph/0304150, hep-ph/0307050, hep-ph/0311172
No oscillationsNo oscillations
Oscillations in SN envelopeOscillations in SN envelope
Earth effects includedEarth effects included
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
One detector observes SN shadowed by EarthOne detector observes SN shadowed by Earth
Model-Independent Strategies for Observing Model-Independent Strategies for Observing Earth EffectsEarth Effects
Case 1:Case 1:• Another detectorAnother detector observes SN directlyobserves SN directly• Identify Earth effectsIdentify Earth effects by comparing signalsby comparing signals
Dighe, Keil & Raffelt, “Identifying Earth matterDighe, Keil & Raffelt, “Identifying Earth mattereffects on supernova neutrinos at a single detector”effects on supernova neutrinos at a single detector”[hep-ph/0304150][hep-ph/0304150]
Case2: Identify “wiggles” in signal of single detectorCase2: Identify “wiggles” in signal of single detector Problem: Smearing by limited energy resolutionProblem: Smearing by limited energy resolution
Water CherenkovWater Cherenkov Need megaton detectorNeed megaton detector
with ~ 10with ~ 105 5 eventsevents
Scintillator detectorScintillator detector ~ 2000 events~ 2000 events may be enoughmay be enough
If 13-mixing angle isIf 13-mixing angle isknown to be “large”,known to be “large”,e.g.e.g. fromfrom DoubleDouble Chooz,Chooz,observed “wiggles” inobserved “wiggles” inenergy spectrum signifyenergy spectrum signifynormal mass hierarchynormal mass hierarchy
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Shock Propagation and Neutrino Supernova Shock Propagation and Neutrino OscillationsOscillations
Schirato & Fuller:Schirato & Fuller:Connection betweenConnection betweensupernova shocks,supernova shocks,flavor transformation,flavor transformation,and the neutrino signaland the neutrino signal[astro-ph/0205390][astro-ph/0205390]
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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,MeV15E
xe
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrinos 20 Jahre nach SN 1987ASupernova Neutrinos 20 Jahre nach SN 1987A
Collective Supernova Neutrino OscillationsCollective Supernova Neutrino Oscillations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrino Density Streaming off a Supernova Neutrino Density Streaming off a Supernova CoreCore
Typical luminosity in oneTypical luminosity in oneneutrino speciesneutrino species
Corresponds to a neutrinoCorresponds to a neutrinonumber density ofnumber density of
Current-current structureCurrent-current structureof weak interactionof weak interactioncauses suppression ofcauses suppression ofeffective potential foreffective potential forcollinear-moving particlescollinear-moving particles
Nu-nu refractive effectNu-nu refractive effectdecreases asdecreases as
Appears to be negligibleAppears to be negligible
serg52103L serg52103L
2335
Rkm
cm103n
2
335R
kmcm103n
Equivalent Neutrino density ∝ R
Nu-nu refraction ∝ R
)cos1(GV Fweak )cos1(GV Fweak
4RV 4RV
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Collective Effects in Neutrino Flavor Collective Effects in Neutrino Flavor OscillationsOscillationsCollapsed supernova core or accretion torus ofCollapsed supernova core or accretion torus ofmerging neutron stars:merging neutron stars:
• Neutrino flux very dense: Up to 10Neutrino flux very dense: Up to 103535 cm cm3 3
• Neutrino-neutrino interaction energy Neutrino-neutrino interaction energy much larger than vacuum oscillation frequencymuch larger than vacuum oscillation frequency• Large “matter effect” of neutrinos on eachLarge “matter effect” of neutrinos on each otherother• Non-linear oscillation effectsNon-linear oscillation effects
• 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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Survival probability Survival probability eeSurvival probability Survival probability ee
NormalNormalHierarchyHierarchy
atm atm mm22
1313closeclose
to Choozto Choozlimitlimit
InvertedInvertedHierarchyHierarchy
NoNonu-nu effectnu-nu effect
NoNonu-nu effectnu-nu effect
Self-Induced Flavor Oscillations of SN Self-Induced Flavor Oscillations of SN NeutrinosNeutrinos
RealisticRealisticnu-nu effectnu-nu effect
BipolarBipolarcollectivecollectiveoscillationsoscillations(single-angle(single-angle approximation)approximation)
MSWMSW
RealisticRealisticnu-nu effectnu-nu effect
MSWMSWeffecteffect
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Mass Hierarchy at Extremely Small Theta-13Mass Hierarchy at Extremely Small Theta-13
Dasgupta, Dighe & Mirizzi, arXiv:0802.1481Dasgupta, Dighe & Mirizzi, arXiv:0802.1481
Ratio of spectra inRatio of spectra intwo water Cherenkovtwo water Cherenkovdetectors (0.4 Mton),detectors (0.4 Mton),one shadowed by theone shadowed by theEarth, the other notEarth, the other not
Using Earth matter effects to diagnose transformationsUsing Earth matter effects to diagnose transformations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (I)(I)
““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
• Sawyer, hep-ph/0408265, 0503013 Sawyer, hep-ph/0408265, 0503013 • Raffelt & Sigl, hep-ph/0701182Raffelt & Sigl, hep-ph/0701182• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, 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, 0709.4641 arXiv:0705.1830, 0709.4641 • 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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Collective SN neutrino oscillations 2006-2008 Collective SN neutrino oscillations 2006-2008 (II)(II)
Second-order mu-tau refractive effectSecond-order mu-tau refractive effectimportant in three-flavor contextimportant in three-flavor context
• Esteban-Pretel, Pastor, Tomàs,Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0712.1137Raffelt & Sigl, arXiv:0712.1137
Three-flavor effects in O-Ne-Mg SNeThree-flavor effects in O-Ne-Mg SNeon neutronization burston neutronization burst(MSW-prepared spectral double split)(MSW-prepared spectral double split)
• Duan, Fuller, Carlson & Qian,Duan, Fuller, Carlson & Qian, arXiv:0710.1271arXiv:0710.1271• Dasgupta, Dighe, Mirrizzi & Raffelt,Dasgupta, Dighe, Mirrizzi & Raffelt, arXiv:0801.1660arXiv:0801.1660
Theory of three-flavor collectiveTheory of three-flavor collectiveoscillationsoscillations
• Dasgupta & Dighe,Dasgupta & Dighe, arXiv:0712.3798arXiv:0712.3798
Identifying the neutrino mass hierarchyIdentifying the neutrino mass hierarchyat extremely small Theta-13at extremely small Theta-13
• Dasgupta, Dighe & Mirizzi,Dasgupta, Dighe & Mirizzi, arXiv:0802.1481 arXiv:0802.1481
But for high density, conversionsBut for high density, conversionssuppressed by geometric effectsuppressed by geometric effect
• Esteban-Pretel, Mirizzi, Pastor,Esteban-Pretel, Mirizzi, Pastor, Tomàs, Raffelt, Serpico & Sigl,Tomàs, Raffelt, Serpico & Sigl, arXiv:0807.0659arXiv:0807.0659
Collective oscillations along flux linesCollective oscillations along flux linesfor non-spherical geometryfor non-spherical geometry
• Dasgupta, Dighe, Mirizzi & Raffelt,Dasgupta, Dighe, Mirizzi & Raffelt, arXiv:0805.3300arXiv:0805.3300
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Neutrino Oscillations in a Neutrino Background Neutrino Oscillations in a Neutrino Background
ff
ZZ
W, ZW, Z
ff
e
n21
n21
eF
2e
n0
0nnG2
E2M
ti
e
n21
n21
eF
2e
n0
0nnG2
E2M
ti
Neutrinos in a mediumNeutrinos in a mediumsuffer flavor-dependentsuffer flavor-dependentrefractionrefraction(Wolfenstein,(Wolfenstein, PRD 17:2369, 1978) PRD 17:2369, 1978)
ZZ
eF
2en2nn
nnn2G2
E2M
ti
ee
ee
eF
2en2nn
nnn2G2
E2M
ti
ee
ee
If neutrinos form theIf neutrinos form thebackground, thebackground, therefractive index hasrefractive index has““offdiagonal elements”offdiagonal elements”(Pantaleone,(Pantaleone, PLB 287:128, 1992)PLB 287:128, 1992)
• One can not operationally distinguish betweenOne can not operationally distinguish between “ “beam” and “background”beam” and “background”• Problem is fundamentally nonlinearProblem is fundamentally nonlinear
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
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”
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
General Equations of MotionGeneral Equations of Motion
]),)[(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 pqqqp3
3
FpFp
2
pt
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
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Oscillations of Neutrinos plus Antineutrinos in Oscillations of Neutrinos plus Antineutrinos in a Boxa Box
Equal and densities, single energy E, withEqual and densities, single energy E, withee ee E2m
nG22
F e
E2m
nG22
F e ≫≫
P)PP(PBPt P)PP(PBPt
EqualEqualself termsself terms
P)PP(PBPt P)PP(PBPt
)()(
)()(
Opposite vacuumOpposite vacuumoscillationsoscillations
PPPP
BB
PP
PP
BB
““Pendulum in flavor space”Pendulum in flavor space”• Inverted mass hierarchyInverted mass hierarchy Inverted pendulumInverted pendulum UnstableUnstable eveneven forfor smallsmall mixingmixing angleangle• Normal mass hierarchyNormal mass hierarchy Small-amplitude oscillationsSmall-amplitude oscillations
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Flavor Conversion Without Flavor Mixing?Flavor Conversion Without Flavor Mixing?
• This is no real “flavor conversion”,This is no real “flavor conversion”, rather a “coherent pair conversion”rather a “coherent pair conversion”
• Occurs anyway at second order GOccurs anyway at second order GFF
• Coherent “speed-up effect” (Sawyer)Coherent “speed-up effect” (Sawyer)
Equal Equal ee and and ee densities in a box densities in a box
(inverted hierarchy)(inverted hierarchy)
Inverted pendulum:Inverted pendulum:• Time to fall dependsTime to fall depends logarithmically onlogarithmically on small initial angle small initial angle • Stays up forever onlyStays up forever only for for = 0 = 0• Unstable by quantumUnstable by quantum uncertainty relationuncertainty relation (“How long can a pencil(“How long can a pencil stand on its tip?”)stand on its tip?”)
ee ee
Not clear (to me) if coherentNot clear (to me) if coherenttransformations can be triggeredtransformations can be triggeredby quantum fluctuations aloneby quantum fluctuations alone(mixing angle (mixing angle = 0) = 0)
__
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Supernova Neutrino ConversionSupernova Neutrino Conversion
NeutrinosNeutrinosin a boxin a box
NeutrinosNeutrinosstreamingstreamingoff a off a supernovasupernovacorecore
Permanent pendularPermanent pendularoscillationsoscillations
Complete conversionComplete conversion• Nu-nu interaction energyNu-nu interaction energy decreasesdecreases• Pendulum’s moment ofPendulum’s moment of inertia inertia 11 increases increases
• Conservation of angular Conservation of angular momentummomentum kinetic energy decreaseskinetic energy decreases amplitude decreases amplitude decreases ∝∝ 1/21/2
nG2 F nG2 F
Envelope Envelope declinesdeclinesas as ∝∝ 1/21/2 ∝∝ rr
22
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Flavor Conversion in Toy SupernovaFlavor Conversion in Toy Supernova
PendularOscillations
• 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)
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Synchronized vs. Pendular OscillationsSynchronized vs. Pendular Oscillations
• Ensemble of unequal densities (antineutrino fraction Ensemble of unequal densities (antineutrino fraction < 1< 1) ) • Equal energies (equal oscillation frequency Equal energies (equal oscillation frequency mm22/2E/2E))• Interaction energy Interaction energy
eenn eenn
enG2 F enG2 F
Free oscillationsFree oscillations
≪≪
PP
PP
BB
Pendular oscillationsPendular oscillations
2)1(
1
2)1(
1≪≪ ≪≪
PP
PP
)1( )1(
BB
Synchronized oscillationsSynchronized oscillations
2)1(
1
2)1(
1≪≪
PP
PP
11
synch
11
synch
BB
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Synchronized vs. Pendular OscillationsSynchronized vs. Pendular Oscillations
Free oscillationsFree oscillations
≪≪
PP
PP
BB
Pendular oscillationsPendular oscillations
2)1(
1
2)1(
1≪≪ ≪≪
PP
PP
)1( )1(
BB
Synchronized oscillationsSynchronized oscillations
2)1(
1
2)1(
1≪≪
PP
PP
11
synch
11
synch
BB
SupernovaSupernovaCoreCore R = 40R = 4060 km60 km R R 200 km 200 km
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Pendulum in Flavor SpacePendulum in Flavor Space
Mass directionMass directionin flavor spacein flavor space
PrecessionPrecession(synchronized oscillation)(synchronized oscillation)
NutationNutation(pendular(pendular oscillation)oscillation)
SpinSpin(Lepton Asymmetry)(Lepton Asymmetry)
• Very asymmetric systemVery asymmetric system - Large spin - Large spin - Almost pure precession - Almost pure precession - Fully synchronized oscillations- Fully synchronized oscillations
• Perfectly symmetric systemPerfectly symmetric system - No spin- No spin - Simple spherical pendulum- Simple spherical pendulum - Fully pendular oscillation- Fully pendular oscillation
[Hannestad, Raffelt, Sigl, Wong:[Hannestad, Raffelt, Sigl, Wong: astro-ph/0608695]astro-ph/0608695]
nn nn
Polarization vectorPolarization vectorfor neutrinos plusfor neutrinos plusantineutrinos antineutrinos
nn nn
≫≫
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Multi-Energy and Multi-Angle EffectsMulti-Energy and Multi-Angle Effects
pqqpq3
3
Fpp
2
pt P)PP)(cos1(2
qdG2PLPB
p2m
P
pqqpq3
3
Fpp
2
pt P)PP)(cos1(2
qdG2PLPB
p2m
P
pqqpq3
3
Fpp
2
pt P)PP)(cos1(2
qdG2PLPB
p2m
P
pqqpq3
3
Fpp
2
pt P)PP)(cos1(2
qdG2PLPB
p2m
P
)()(
)()(
• Different modes oscillateDifferent modes oscillate with different frequencieswith different frequencies kinematical decoherencekinematical decoherence
• Self-maintained coherenceSelf-maintained coherence by nu-nu interactionsby nu-nu interactions
• Can lead to “spectral split”Can lead to “spectral split”
Isotropic matter backgroundIsotropic matter backgroundaffects all modes the sameaffects all modes the same
Multi-angle effects for non-isotropicMulti-angle effects for non-isotropicnu distribution (streaming from SN):nu distribution (streaming from SN):Different modes should oscillateDifferent modes should oscillatedifferently differently kinematical decoherence kinematical decoherenceHowever, nu-nu interaction can lead toHowever, nu-nu interaction can lead to
• “ “Angular synchronization”Angular synchronization” (quasi-single angle behavior)(quasi-single angle behavior)
• Self-accelerated multi-angleSelf-accelerated multi-angle decoherencedecoherence
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Spectral Split (Stepwise Spectral Swapping)Spectral Split (Stepwise Spectral Swapping)
Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998Fogli, Lisi, Marrone & Mirizzi, arXiv:0707.1998
Initial fluxesInitial fluxesat nu sphereat nu sphere
AfterAftercollectivecollectivetrans-trans-formationformation
For explanation seeFor explanation see
Raffelt & SmirnovRaffelt & SmirnovarXiv:0705.1830arXiv:0705.1830 0709.46410709.4641
Duan, Fuller,Duan, Fuller,Carlson & QianCarlson & QianarXiv:0706.4293arXiv:0706.4293 0707.02900707.0290
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
Spectral split in terms of the Spectral split in terms of the variable variable
initial
initial
final
final
Collective conversion of thermal spectra of Collective conversion of thermal spectra of ee and and ee as in a supernova as in a supernova__
Energy spectrumEnergy spectrum Spectrum in terms of Spectrum in terms of mm22/2E/2E
Flavor lepton number conservation:Flavor lepton number conservation:Equal integralsEqual integrals
Raffelt & Smirnov, arXiv:0709.4641Raffelt & Smirnov, arXiv:0709.4641
initialinitial
final final
Georg Raffelt, Max-Planck-Institut für Physik, München, Germany Neutrino Physics & Astrophysics, 17-21 Sept 2008, Beijing, China
SN 1006SN 1006
Looking forward to the next galactic supernovaLooking forward to the next galactic supernova
http://antwrp.gsfc.nasa.gov/apod/ap060430.htmlhttp://antwrp.gsfc.nasa.gov/apod/ap060430.html
May take a long timeMay take a long timeNo problemNo problemLots of theoretical work to do!Lots of theoretical work to do!