Georg Raffelt, Max-Planck-Institut für Physik, München Totsuka Memorial Symposium, 9 June 2009, Tokyo Supernova Neutrinos Supernova Neutrinos Georg Raffelt, Max-Planck-Institut für Georg Raffelt, Max-Planck-Institut für Physik, München Physik, München Yoji Totsuka Memorial Symposiu Yoji Totsuka Memorial Symposium 9 June 2009, University of Tokyo 9 June 2009, University of Tokyo
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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
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
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]
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.
The gravitational-wave signal from convectionThe gravitational-wave signal from convectionis a generic and dominating featureis a generic and dominating feature
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
• 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
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
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