Outline

2. Outline Collective Swaps MSW Conversions www.ps.uci.edu/~tomba/sk/tscan Neutrino Production Neutrino Propagation and Flavor Conversion Neutrino Detection Neutrino Astronomy Supernova Astrophysics Neutrino Masses & Mixing Other properties Pointing in advance/SN alerts Signatures of stellar dynamics Tracking the local SN rate R-process nucleosynthesis Neutrino Mass Hierarchy Q13 estimate Sub-leading/Non-Standard effects Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

3. Neutrino Production in Supernovae

4. SN Explosion and Neutrino Emission Main-sequence star Onion structure Collapse (implosion) Helium-burning star Helium Burning Hydrogen Burning Hydrogen Burning Degenerate iron core: r 109 g cm-3 T 1010 K MFe 1.5 Msun RFe 8000 km Adapted from a slide by Georg Raffelt Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

5. SN Explosion and Neutrino Emission Newborn Neutron Star ~ 50 km Proto-Neutron Star rrnuc = 3 1014 g cm-3 T  30 MeV Collapse (implosion) Bounce (explosion) Prompt Shock Stalls Neutrino Heating Neutrino Driven Explosion ne Burst Neutrino Cooling Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

6. Neutrino Luminosities and Energies Burst Phase Accretion Phase Luminosity in1051erg/s • For ne, anti-ne and nx Cooling Phase Average Energy inMeV • For ne, anti-ne and nx Raffelt, Keil, Buras, Janka and Rampp, arXiv:astro-ph/0303226 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

7. Neutrino Luminosities and Energies Luminosity in1051erg/s For ne and anti-ne Luminosity in1051erg/s For nx (non-electron) RMS Energy in MeV • For ne, anti-ne and nx Fischer et al. (Basel Group),arXiv:0904.1871 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

8. Neutrino Propagation and Flavor Conversions

9. Free-Streaming Neutrinos Nonlinear nu-nu effects are important when nu-nu interaction energy exceeds the typical vacuum oscillation frequency These interactions give rise to “Collective” flavor conversions • Vacuum oscillations • M is neutrino mass matrix • Overall minus sign for • antineutrinos MSW effect depends on ordinary matter density L, i.e. mainly electron density Nonlinear Effects depends on the neutrino density r Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

10. Collective Flavor Conversion Neutrino pair-conversions 1 1 Pee Pee L Synchronized Oscillations L Pantaleone (PLB, 1992) 0 0 Neutrinos of all energies oscillate together. Neutrinos of all energies flip to the lighter mass eigenstate. Bipolar Oscillations Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

11. Collective Flavor Conversion Instability in Flavor Space  Swap around spectral crossings Initial Final  e  e Swap cannot be complete, because of Total Lepton Number Conservation Flavor Fluxes Energy Energy Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

12. Spectral Swaps/Splits Dasgupta, Dighe, Raffelt and Smirnov, arXiv:0904.3542 (PRL) For movies see http://www.mppmu.mpg.de/supernova/multisplits Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

13. Spectral Swaps/Splits Dasgupta, Dighe, Raffelt and Smirnov, arXiv:0904.3542 (PRL) For movies see http://www.mppmu.mpg.de/supernova/multisplits Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

14. Spectral Swaps: Accretion Phase Nontrivial Evolution only for Inverted Hierarchy Fogli, Lisi, Marrone and Mirizzi, arXiv: 0707.1998 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

15. Spectral Swaps: Cooling Phase Spectral Splits in Inverted Hierarchy Spectral Splits in Normal Hierarchy Dasgupta, Dighe, Raffelt and Smirnov, arXiv: 0904.3542 (PRL) Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

16. 3 Flavor Spectral Swaps: Cooling Phase NH IH Friedland, arXiv:1001.0996 Dasgupta, Mirizzi, Tamborra and Tomas, arXiv:1002.2943 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

17. Lot of activity in recent years Seminal papers: Duan, Fuller, Carlson and Qian in 2005, 2006 Pendulum Analogy: Hannestad, Raffelt, Sigl and Wong, arXiv:astro-ph/0608695 More than 100 papers on collective effects by: Abazajian, Balantekin, Beacom, Bell, Blennow, Carlson, Dasgupta, Dighe, Dolgov, Duan, Esteban-Pretel, Fogli, Friedland, Fuller, Gava, Goswami, Hannestad, Hansen, Kneller, Kostelecky, Lisi, Lunardini, Marrone, McLaughlin, Mirizzi, Pantaleone, Pastor, Pehlivan, Qian, Raffelt, Samuel, Serpico, Semikoz, Sigl, Smirnov, Stodolsky, Tomas, Volpe, Wong… Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

18. MSW conversions in SN NH IH Dighe and Smirnov, arXiv: hep-ph/9907423 • H resonance : n1/n2n3 (Dmatm2 , q13) at 103 – 104g/cc • In neutrinos for NH and in antineutrinos for IH. • Adiabaticity ≈ sin2q13 Spectral Splits in • L resonance : n1n2 • (Dmsol2 , q12) at 101 – 102g/cc • Always in neutrinos. Always adiabatic. Spectral Splits in Inverted Hierarchy Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

19. Regeneration in Earth Matter Electron flavor flux = cos212 1 + sin2 12 2 L Detector Location Matters! Electron flavor: = (1-P2e) 1 + P2e 2 P2eis the probability of 2 toe which depends on Earth density and L Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

20. Survival Probabilities B. Dasgupta,arXiv:hep-ph/1005.2681 [Moriond-2010, Proceedings] Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

21. Neutrino Detection

22. Running (soon) SN Neutrino Detectors SNO+ Baksan HALO Icarus ✔ Mini-BOONE Daya-Bay Super-K LVD Borexino KamLAND ✔ NOnA ✔ Icecube Hyper-K/UNO/DUSEL/LENA/Km3NET/… ✔=Large (>103 events for 10kpc SN) Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

23. Main Detection Channels • SK-like water Cherenkov detector (30 kt, SN at 10kpc) • Scintillation detector • Liquid Argon detector Super-Kamiokande and Icecube are at present our largest detectors for SN neutrinos. Liquid Argon TPC can see neutrinos, others mostly see antineutrinos Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

24. Gadzooks ne can be identified by delayed coincidence. Gadolinium Anti-nu Detector Zealously Outperforming Old Kamiokande. Super! n g ne p p n+Gd→ ~8 MeVg(90%) n+p→ d + 2.2 MeVg(10%) Gd e+ g Positron and gamma ray vertices are within ~50cm. Can identify each antineutrino on an event-by-event basis [reaction schematic by M. Nakahata] Beacom and Vagins, arXiv:hep-ph/0309300 (PRL) Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

25. What Can We Learn ?

26. SN pointing alerts/SNEWS • Neutrinos reach ~24 hours before the light from SN explosion • SN at 10 kpc may be detected within a cone of ∼ 5◦ at SK, factor of 3 better with Gd, and factor of 10 better with a 30xSK Beacom and Vogel,arXiv: astro-ph/9811350 Tomas, Semikoz, Kachelriess, Raffelt and Dighe, arXiv: hep-ph/0307050 This may be crucial for dust-obscured supernovae! Coincidence at multiple detectors will trigger an alert for astronomers SNEWS http://snews.bnl.gov Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

27. Stellar Explosion Dynamics Standing Accretion Shock Instability Large scale motion of the stellar material on a millisecond timescale Fluctuations in the neutrino signal, luminosities and energies Lund, Marek, Lunardini, Janka andRaffelt:astro-ph/1006.1889 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

28. Diffuse Neutrino Background Guaranteed source of neutrinos from cosmological distances Estimated present-day flux from all SN in our past~ 10 cm-2 s-1 Beacom and Vagins, hep-ph/0309300 (PRL) Horiuchi, Beacom and Dwek, arXiv:0812.3157 See also Chakraborty, Choubey, Dasgupta and Kar, arXiv:0805.3131 for effect of collective oscillations on DSNB Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

29. Q13Estimate/Shockwave effects Tomas, Kachelriess, Dighe, Raffelt and Janka, arXiv:astro-ph/0407132 Most of the work on this was done around 2000-2004 Needs to be re-done after including collective effects e.g. Gava, Kneller, Volpe and Mc Laughlin, arXiv:0902.0317 (PRL) Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

30. Neutrino Mass Hierarchy Ratio of events at two 0.4 MT WC detectors, one shadowed and other not. SN taken at 10 kpc. Dasgupta, Dighe and Mirizzi, arXiv: arXiv:0802.1481 (PRL) Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

31. Steps ahead… • Angle-dependent simulations with cooling fluxes, e.g. Duan and Friedland: hep-ph/1006.2359. More needed… • Anisotropic neutrino emission… • More clear analytical understanding… • ??? Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

32. Summary Collective Swaps MSW Conversions www.ps.uci.edu/~tomba/sk/tscan Neutrino Production Neutrino Propagation and Flavor Conversion Neutrino Detection Neutrino Astronomy Supernova Astrophysics Neutrino Masses & Mixing Other properties Pointing in advance/SN alerts Signatures of stellar dynamics Tracking the local SN rate R-process nucleosynthesis Neutrino Mass Hierarchy Q13 estimate Sub-leading/Non-Standard effects A rare event is a lifetime opportunity Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

33. Back-up Slide 1: R-process nucleosynthesis Demanding successful R-process nucleosynthesis puts non-trivial constraints on possible SN fluxes. Chakraborty, Choubey, Goswami and KararXiv: arXiv:0911.1218 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010

34. Back-up Slide 2: Non-Standard effects Non-Standard Interactions can give rise to a rich set of possibilities, and make things more complicated. Esteban-Pretel, Tomas and Valle, arXiv:0909.2196 Basudeb Dasgupta, PPC-2010 at Torino, Italy, 12 - 16 July 2010