Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Supernova NeutrinosSupernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, Georg Raffelt, Max-Planck-Institut für Physik, MünchenMünchen
Yoji Totsuka Memorial SymposiumYoji Totsuka Memorial Symposium9 June 2009, University of Tokyo9 June 2009, University of Tokyo
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Supernova NeutrinosSupernova Neutrinos
Supernova NeutrinosSupernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Diffuse Supernova Neutrino Background Diffuse Supernova Neutrino Background (DSNB)(DSNB)
Supernova rate approximatelySupernova rate approximately
1 SN / 101 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 erg per core-collapse
Core-collapse neutrino luminosity ofCore-collapse neutrino luminosity oftypical galaxy comparable to photontypical galaxy comparable to photonluminosity (from nuclear burning) luminosity (from nuclear burning)
Core-collapse rate somewhat largerCore-collapse rate somewhat largerin the past. Estimated present-dayin the past. Estimated present-day
flux ~ 10 cmflux ~ 10 cm11 s s11ee
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
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Gamow & Schoenberg, Phys. Rev. 58:1117 Gamow & Schoenberg, Phys. Rev. 58:1117 (1940)(1940)
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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. Alekseev et al., Astrophys. 288 (1994) L1. Tammann et al., ApJ 92 (1994) 487. Alekseev et al., JETP 77 (1993) 339 and my update.JETP 77 (1993) 339 and my update.
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
High and Low Supernova Rates in Nearby High and Low Supernova Rates in Nearby GalaxiesGalaxies
M31 (Andromeda)M31 (Andromeda)D = 780 kpcD = 780 kpc
Last Observed Supernova: 1885ALast Observed Supernova: 1885A
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Super-Kamiokande Neutrino DetectorSuper-Kamiokande Neutrino Detector
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
IceCube Neutrino Telescope at the South PoleIceCube Neutrino Telescope at the South Pole
• 1 km1 km33 antarctic ice, instrumented antarctic ice, instrumented with 4800 photomultiplierswith 4800 photomultipliers• 59 of 80 strings installed (2009)59 of 80 strings installed (2009)• Completion until 2011 foreseenCompletion until 2011 foreseen
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 < 300 Hz< 300 Hz
• Total ofTotal of 4800 Oms4800 Oms foreseenforeseen in IceCubein IceCube
IceCube SN signal at 10 kpc, basedIceCube SN signal at 10 kpc, basedon a numerical Livermore modelon a numerical Livermore model[Dighe, Keil & Raffelt, hep-ph/0303210][Dighe, Keil & Raffelt, hep-ph/0303210]
Method first discussed byMethod first discussed by• Pryor, Roos & Webster,Pryor, Roos & Webster, ApJ 329:355 (1988)ApJ 329:355 (1988)• Halzen, Jacobsen & ZasHalzen, Jacobsen & Zas astro-ph/9512080astro-ph/9512080
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
LAGUNA - Ongoing European (FP7) Design LAGUNA - Ongoing European (FP7) Design StudyStudy
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Reaching Beyond the Milky Way: Five-Megaton Reaching Beyond the Milky Way: Five-Megaton DetectorDetector
Modular 5-Mt underwater detector Modular 5-Mt underwater detector for proton decay, long-baseline oscillation experiments,for proton decay, long-baseline oscillation experiments,atmospheric neutrinos, and low-energy burst detectionatmospheric neutrinos, and low-energy burst detection
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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.
CoincidenceCoincidenceServer Server @ BNL@ BNL
Super-KSuper-K
AlertAlert
Others ?Others ?
LVDLVD
IceCubeIceCube
Supernova 1987ASupernova 1987AEarly Light CurveEarly Light Curve http://snews.bnl.gov
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Looking forwardLooking forward
Probing Supernova PhysicsProbing Supernova Physics
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Luminosity Variation Detectable in Neutrinos?Luminosity Variation Detectable in Neutrinos?
Marek, Janka & MMarek, Janka & Müüller, arXiv:0808.4136ller, arXiv:0808.4136
Hemispheric averagePolar direction
Neutrino events in 10 ms bins forNeutrino events in 10 ms bins forSN (10 kpc) during accretion phase:SN (10 kpc) during accretion phase:
• Super-K 70 1Super-K 70 1 ~ 10% ~ 10%• 30 x Super-K 230 x Super-K 210103 3 11 ~ ~ 2%2%• IceCube IceCube 1110104 4 11 ~ ~ 1%1%
Detecting the spectrum of luminosityDetecting the spectrum of luminosityvariations canvariations can• Detect SASI instability in neutrinosDetect SASI instability in neutrinos• Provide equation-of-stateProvide equation-of-state informationinformation
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Looking forwardLooking forward
Flavor Oscillations of Flavor Oscillations of Supernova NeutrinosSupernova Neutrinos
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Neutrino Flavor OscillationsNeutrino Flavor Oscillations
Two-flavor mixingTwo-flavor mixing
2
1e
cossin
sincos
2
1e
cossin
sincos
Bruno PontecorvoBruno Pontecorvo(1913 – 1993)(1913 – 1993)
Invented nu oscillationsInvented nu oscillations
Each mass eigenstate propagates asEach mass eigenstate propagates as
with with
ipzeipze
E2m
EmEp2
22 E2
mEmEp
222
zE2
m2z
E2m2
Phase difference implies flavor oscillationsPhase difference implies flavor oscillations
Oscillation Oscillation LengthLength
2
2
2 m
eVMeVE
m5.2m
E4
2
2
2 m
eVMeVE
m5.2m
E4
sinsin22(2(2))
ProbabilityProbability ee
zz
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Three-Flavor Neutrino ParametersThree-Flavor Neutrino Parameters
3
2
1
1212
1212
1313
1313
2323
2323
e
1
CS
SC
CS
1
SC
CS
SC
1
3
2
1
1212
1212
1313
1313
2323
2323
e
1
CS
SC
CS
1
SC
CS
SC
1 ie ie
ie ie
.,etccosC 1212 .,etccosC 1212 CP-violating phaseCP-violating phase
SolarSolar75759292
AtmosphericAtmospheric1400140030003000
22 meVm 22 meVm
CHOOZCHOOZ Solar/KamLANDSolar/KamLAND 22 ranges rangeshep-ph/0405172hep-ph/0405172
Atmospheric/K2KAtmospheric/K2K 5437 23 5437 23 1113 1113 3630 12 3630 12
ee
ee
11SunSun
NormalNormal
22
33
AtmosphereAtmosphere
ee
ee
11SunSun
InvertedInverted22
33
AtmosphereAtmosphere
Tasks and Open QuestionsTasks and Open Questions
• Precision for Precision for 12 12 andand 2323
• How large is How large is 1313 ??
• CP-violating phase CP-violating phase ??• Mass orderingMass ordering ? ? (normal vs inverted)(normal vs inverted)• Absolute massesAbsolute masses ?? (hierarchical vs degenerate)(hierarchical vs degenerate)• Dirac or MajoranaDirac or Majorana ??
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Neutrino Oscillations in MatterNeutrino Oscillations in Matter
• “ “Level crossing” possible in a medium with a gradient (MSW effect)Level crossing” possible in a medium with a gradient (MSW effect) - For solar nus large flavor conversion anyway due to large mixing- For solar nus large flavor conversion anyway due to large mixing - Still important for 13-oscillations in supernova envelope- Still important for 13-oscillations in supernova envelope• Breaks degeneracy between Breaks degeneracy between and and /2 /2 (dark vs light side) (dark vs light side) - 12 mass ordering for solar nus established- 12 mass ordering for solar nus established - 13 mass ordering (normal vs inverted) at future LBL or SN- 13 mass ordering (normal vs inverted) at future LBL or SN• Discriminates against sterile nus in atmospheric oscillationsDiscriminates against sterile nus in atmospheric oscillations• CP asymmetry in LBL, to be distinguished from intrinsic CP violationCP asymmetry in LBL, to be distinguished from intrinsic CP violation• Prevents flavor conversion in a SN core and within shock wavePrevents flavor conversion in a SN core and within shock wave• Strongly affects sterile nu production in SN or early universeStrongly affects sterile nu production in SN or early universe
Lincoln WolfensteinLincoln Wolfenstein
ff
ZZ
W, ZW, Z
ff
Neutrinos in a medium suffer flavor-dependentNeutrinos in a medium suffer flavor-dependentrefraction (PRD 17:2369, 1978)refraction (PRD 17:2369, 1978)
e
n21
n21
eF
2e
n0
0nnG2
E2M
zi
e
n21
n21
eF
2e
n0
0nnG2
E2M
zi
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Shockwave Effects in a Megaton Cherenkov Shockwave Effects in a Megaton Cherenkov DetectorDetector
8.0)(Flux)(Flux
x
e
8.0)(Flux)(Flux
x
e
MeV18)(E
MeV15)(E
x0
e0
MeV18)(E
MeV15)(E
x0
e0
5.0)(Flux)(Flux
x
e
5.0)(Flux)(Flux
x
e
MeV15)(E
MeV15)(E
x0
e0
MeV15)(E
MeV15)(E
x0
e0
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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
Non-linear neutrino-neutrinoeffect is important, evenif matter density is large
Non-linear neutrino-neutrinoeffect is important, evenif matter density is large
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Collective SN Neutrino Oscillations since 2006Collective SN Neutrino Oscillations since 2006
Two seminal papers in 2006 triggered a torrent of activitiesDuan, Fuller, Qian, astro-ph/0511275, Duan et al. astro-ph/0606616
Duan, Fuller, Carlson & Qian, astro-ph/0608050, 0703776, arXiv:0707.0290, 0710.1271. Duan, Fuller & Qian, arXiv:0706.4293, 0801.1363, 0808.2046. Duan, Fuller & Carlson, arXiv:0803.3650. Duan & Kneller, arXiv:0904.0974. Hannestad, Raffelt, Sigl & Wong, astro-ph/0608695. Balantekin & Pehlivan,astro-ph/0607527. Balantekin, Gava & Volpe, arXiv:0710.3112. Gava & Volpe,arXiv:0807.3418. Gava, Kneller, Volpe & McLaughlin, arXiv:0902.0317. Raffelt & Sigl, hep-ph/0701182. Raffelt & Smirnov, arXiv:0705.1830,0709.4641. Esteban-Pretel, Pastor, Tomàs, Raffelt & Sigl, arXiv:0706.2498,0712.1137. Esteban-Pretel, Mirizzi, Pastor, Tomàs, Raffelt, Serpico & Sigl,arXiv:0807.0659. Raffelt, arXiv:0810.1407. Fogli, Lisi, Marrone & Mirizzi,arXiv:0707.1998. Fogli, Lisi, Marrone & Tamborra, arXiv:0812.3031. Lunardini, Müller & Janka, arXiv:0712.3000. Dasgupta & Dighe, arXiv:0712.3798. Dasgupta, Dighe & Mirizzi, arXiv:0802.1481. Dasgupta,Dighe, Mirizzi & Raffelt, arXiv:0801.1660, 0805.3300. Dasgupta, Dighe,Raffelt & Smirnov, arXiv:0904.3542. Sawyer, arXiv:0803.4319.Chakraborty, Choubey, Dasgupta & Kar, arXiv:0805.3131. Blennow, Mirizzi &Serpico, arXiv:0810.2297. Wei Liao, arXiv:0904.0075, 0904.2855.
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
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 Totsuka Memorial Symposium, 9 June 2009, Tokyo
Multiple Spectral Splits (Cooling-Phase Multiple Spectral Splits (Cooling-Phase Example)Example)
Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542
ee
xxee xx
InvertedHierarchy
NormalHierarchy
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Multiple Spectral Splits in the Multiple Spectral Splits in the Variable Variable
Dasgupta, Dighe, Raffelt & Smirnov,Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542arXiv:0904.3542
Given is the flux spectrum f(E) forGiven is the flux spectrum f(E) foreach flavoreach flavor
Use Use mm22/2E to label modes/2E to label modes
Label anti-neutrinos with Label anti-neutrinos with
antineutrinos neutrinos
ee
xx
ee
xx
Define “spectrum” asDefine “spectrum” as
)E(f)E(f
)E(f)E(f)(g
ex
xe NeutrinosNeutrinos
AntineutrinosAntineutrinos
Swaps develop around everySwaps develop around every““positive” spectral crossing positive” spectral crossing
Each swap flanked by two splits Each swap flanked by two splits
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Flavor PendulumFlavor Pendulum
Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542For movies see http://www.mppmu.mpg.de/supernova/multisplitsFor movies see http://www.mppmu.mpg.de/supernova/multisplits
Single “positive” crossingSingle “positive” crossing(potential energy at a maximum)(potential energy at a maximum)
Single “negative” crossingSingle “negative” crossing(potential energy at a minimum)(potential energy at a minimum)
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Decreasing Neutrino DensityDecreasing Neutrino Density
Certain initial neutrino densityCertain initial neutrino density Four times smallerFour times smallerinitial neutrino densityinitial neutrino density
Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542For movies see http://www.mppmu.mpg.de/supernova/multisplitsFor movies see http://www.mppmu.mpg.de/supernova/multisplits
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Supernova Cooling-Phase ExampleSupernova Cooling-Phase Example
Normal HierarchyNormal Hierarchy Inverted HierarchyInverted Hierarchy
Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542For movies see http://www.mppmu.mpg.de/supernova/multisplitsFor movies see http://www.mppmu.mpg.de/supernova/multisplits
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Multiple Spectral Splits (Cooling-Phase Multiple Spectral Splits (Cooling-Phase Example)Example)
Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542Dasgupta, Dighe, Raffelt & Smirnov, arXiv:0904.3542
ee
xxee xx
InvertedHierarchy
NormalHierarchy
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Questions and OpportunitiesQuestions and Opportunities
Self-induced collective oscillations occur evenSelf-induced collective oscillations occur even for very small 13-mixing (instability!)for very small 13-mixing (instability!)
Do matter-density fluctuations have anyDo matter-density fluctuations have any realistic impact?realistic impact?
Theoretical understanding and role of Theoretical understanding and role of “ “multi-angle effects” largely missingmulti-angle effects” largely missing
Observation of spectral split or swap indicationObservation of spectral split or swap indication can provide signature for mass hierarchycan provide signature for mass hierarchy and nontrivial neutrino propagation dynamicsand nontrivial neutrino propagation dynamics
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
Looking forwardLooking forward
Looking forward to the next galactic supernovaLooking forward to the next galactic supernovaMay take a long timeMay take a long timeNo problemNo problemLots of theoretical work to do!Lots of theoretical work to do!
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
TotsukaTotsuka
Lots of theoretical work to do!Lots of theoretical work to do!experimentalexperimental
Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo
TotsukaTotsuka
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