Supernova Neutrinos - Department of Theoretical Physics

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Neutrino Burst Observation : First verification of stellar evolution mechanism Neutrino Astronomy
Energy Distribution of SN 1987A Neutrinos Kamiokande-II (Japan) Water Cherenkov detector 2140 tons Irvine-Michigan-Brookhaven (US) Water Cherenkov detector 6800 tons Alessandro Mirizzi JIGSAW 2010 Mumbai, 22-02-2010
Page 1 and 2: JIGSAW 2010 Joint Indo-German Super
Page 3 and 4: NEUTRINOS Neutrino oscillations Neu
Page 5 and 6: WHY SUPERNOVA NEUTRINOS? SN EXPLOSI
Page 7 and 8: Stellar Collapse and Supernova Expl
Page 9 and 10: TYPICAL PROBLEMS IN SUPERNOVA NEUTR
Page 11 and 12: Neutrino spectra (in energy) “qua
Page 13: Sanduleak -69 202 Supernova 1987A 2
Page 17 and 18: NEW LONG-TERM COOLING CALCULATION L
Page 19 and 20: What could we see “tomorrow”? S
Page 21 and 22: Simulated Supernova Signal at Super
Page 23 and 24: SIGNALS OF QCD PHASE TRANSITION IN
Page 25 and 26: Next generation Detectors for Super
Page 27 and 28: NEUTRONIZATION BURST WC Lar TPC I.H
Page 29 and 30: SN n FLAVOR TRANSITIONS The flavor
Page 31 and 32: 3n FRAMEWORK Mixing parameters: U =
Page 33 and 34: MIKHEYEV-SMIRNOV-WOLFENSTEIN (MSW)
Page 35 and 36: events/bin PROBING SHOCK WAVES AND
Page 37 and 38: NEUTRINO-NEUTRINO INTERACTIONS In t
Page 39 and 40: SYNCHRONIZED OSCILLATIONS BY NEUTRI
Page 41 and 42: PENDULUM IN FLAVOR SPACE [Hannestad
Page 43 and 44: NEUTRINO FLUX NUMBERS [Raffelt et a
Page 45 and 46: MULTIPLE SPECTRAL SPLITS IN THE COO
Page 47 and 48: USING EARTH EFFECT TO DIAGNOSE COLL
Page 49 and 50: COLLECTIVE SUPERNOVA NEUTRINO OSCIL
Page 51 and 52: Multiple spectral splits: Dasgupta,
Page 53 and 54: CONCLUSIONS Observing SN neutrinos
Page 55: …WE WILL HAVE NO TIME TO GET BORE

Supernova Neutrinos - Department of Theoretical Physics

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