1. Rencontres de Moriond, 6 -13 March 2010 Electroweak Interactions and Unified Theories Neutrinos from Supernovae Basudeb Dasgupta Max Planck Institute for Physics, Munich

2. Outline Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 www.ps.uci.edu/~tomba/sk/tscan NeutrinoProductionNeutrinoDetection Neutrino Propagation and Flavor Conversion Neutrino Astronomy Supernova Astrophysics Neutrino Masses & Mixing Other properties 1.Pointing in advance/SN alerts 2.Signatures of stellar dynamics 3.Tracking the local SN rate 4.R-process nucleosynthesis 1.Neutrino Mass Hierarchy 2.  13 estimate 3.Sub-leading/Non-Standard effects Collective Swaps MSW Conversions

3. Neutrino Production in Supernovae

4. SN Explosion and Neutrino Emission Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Main-sequence star Hydrogen Burning Helium-burning star HeliumBurning HydrogenBurning Onion structure Degenerate iron core:  10 9 g cm -3  10 9 g cm -3 T  10 10 K T  10 10 K M Fe  1.5 M sun M Fe  1.5 M sun R Fe  8000 km R Fe  8000 km Collapse (implosion) Adapted from a slide by Georg Raffelt

5. SN Explosion and Neutrino Emission Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Collapse (implosion) Bounce (explosion) eBurst Prompt Shock Stalls Neutrino Heating Neutrino Driven Explosion Newborn Neutron Star ~ 50 km Proto-Neutron Star    nuc = 3  10 14 g cm -3 T  30 MeV Neutrino Cooling

6. Neutrino Luminosities and Energies Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Luminosity in 10 51 erg/s For e, anti- e and x Average Energy in MeV For e, anti- e and x Accretion Phase Cooling Phase Cooling Phase Raffelt, Keil, Buras, Janka and Rampp, arXiv:astro-ph/0303226

7. Neutrino Luminosities and Energies Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Fischer et al. (Basel Group),arXiv:0904.1871 Luminosity in 10 51 erg/s For e and anti- e Luminosity in 10 51 erg/s For x (non-electron) RMS Energy in MeV For e, anti- e and x

8. Neutrino Propagation and Flavor Conversions Neutrino Propagation and Flavor Conversions

9. Free-Streaming Neutrinos Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 MSW effect depends on ordinary matter density L, i.e. mainly electron density Vacuum oscillations M is neutrino mass matrix M is neutrino mass matrix Overall minus sign for Overall minus sign forantineutrinos 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 Nonlinear Effects depends on the neutrino density 

10. Lot of activity in recent years Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 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 …

11. Collective Flavor Conversion Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Pantaleone (PLB, 1992) Synchronized Oscillations P ee L 0 1 L 0 1 Bipolar Oscillations Neutrinos of all energies flip to the lighter mass eigenstate. Neutrinos of all energies oscillate together. Neutrino pair-conversions

12. Collective Flavor Conversion Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Swap cannot be complete, because of Total Lepton Number Conservation Instability in Flavor Space  Swap around spectral crossings Flavor Fluxes Energy e e   InitialFinal

13. Spectral Swaps/Splits Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Dasgupta, Dighe, Raffelt and Smirnov, arXiv:0904.3542 (PRL) For movies see http://www.mppmu.mpg.de/supernova/multisplits

14. Spectral Swaps/Splits Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Dasgupta, Dighe, Raffelt and Smirnov, arXiv:0904.3542 (PRL) For movies see http://www.mppmu.mpg.de/supernova/multisplits

15. Spectral Swaps: Accretion Phase Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Fogli, Lisi, Marrone and Mirizzi, arXiv: 0707.1998 Nontrivial Evolution only for Inverted Hierarchy

16. Spectral Swaps: Cooling Phase Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Dasgupta, Dighe, Raffelt and Smirnov, arXiv: 0904.3542 (PRL) Spectral Splits in Inverted Hierarchy Spectral Splits in Normal Hierarchy

17. 3 Flavor Spectral Swaps: Cooling Phase Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Friedland, arXiv:1001.0996 Dasgupta, Mirizzi, Tamborra and Tomas, arXiv:1002.2943 Dasgupta, Mirizzi, Tamborra and Tomas, arXiv:1002.2943 NHIH

18. MSW conversions in SN Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 NHIH Spectral Splits in Inverted Hierarchy Spectral Splits in H resonance : 1 / 2 3 (  m atm 2,  13 ) at 10 3 – 10 4 g/cc In neutrinos for NH and in antineutrinos for IH. Adiabaticity ≈ sin 2  13 Dighe and Smirnov, arXiv: hep-ph/9907423

19. Regeneration in Earth Matter Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Electron flavor flux = cos 2  12 1 + sin 2  12 2 Electron flavor : = (1-P 2e ) 1 + P 2e 2 P 2e is the probability of 2 to e which depends on Earth density and L L Detector Location Matters!

20. Neutrino Detection

21. Running (soon) SN Neutrino Detectors Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Hyper-K/UNO/DUSEL/LENA/Km3NET/… Icecube Super-K KamLAND Mini-BOONE LVD Borexino Baksan IcarusHALO SNO+ NO A ✔ ✔ ✔ ✔ =Large (>10 3 events for 10kpc SN) Daya-Bay

22. Main Detection Channels Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 SK-like water Cherenkov detector (30 kt, SN at 10kpc) Scintillation detector Liquid Argon detector Liquid Argon TPC can see neutrinos others mostly see antineutrinos Super-Kamiokande and Icecube are at present our largest detectors for SN neutrinos.

23. Positron and gamma ray vertices are within ~50cm. [reaction schematic by M. Nakahata] e e+e+ p n   p Gd Gadzooks Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 e can be identified by delayed coincidence. e can be identified by delayed coincidence. n+Gd → ~8 MeV  (90%) n+p → d + 2.2 MeV  (10%) Beacom and Vagins, arXiv:hep-ph/0309300 (PRL) Can identify each antineutrino on an event-by-event basis Gadolinium Anti-nu Detector Zealously Outperforming Old Kamiokande. Super!

24. What Can We Learn ?

25. SN pointing alerts/SNEWS Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Beacom and Vogel, arXiv: astro-ph/9811350 Tomas, Semikoz, Kachelriess, Raffelt and Dighe, arXiv: hep-ph/0307050 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 This may be crucial for dust-obscured supernovae! SNEWShttp://snews.bnl.gov Coincidence at multiple detectors will trigger an alert for astronomers

26. Stellar Explosion Dynamics Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Standing Accretion Shock Instability Large scale motion of the stellar material on a millisecond timescale Fluctuations in the neutrino luminosities and energies Lund, Marek, Lunardini, Janka and Raffelt (in progress)

27. Diffuse Neutrino Background Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 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 Guaranteed source of neutrinos from cosmological distances See also Chakraborty, Choubey, Dasgupta and Kar, arXiv:0805.3131 for effect of collective oscillations on DSNB for effect of collective oscillations on DSNB

28.  13 Estimate/Shockwave effects Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 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)

29. Neutrino Mass Hierarchy Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 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)

30. Summary Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 www.ps.uci.edu/~tomba/sk/tscan NeutrinoProductionNeutrinoDetection Neutrino Propagation and Flavor Conversion Neutrino Astronomy Supernova Astrophysics Neutrino Masses & Mixing Other properties 1.Pointing in advance/SN alerts 2.Signatures of stellar dynamics 3.Tracking the local SN rate 4.R-process nucleosynthesis 1.Neutrino Mass Hierarchy 2.  13 estimate 3.Sub-leading/Non-Standard effects Collective Swaps MSW Conversions A rare event is a lifetime opportunity

31. Back-up Slide 1: R-process nucleosynthesis Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 Demanding successful R-process nucleosynthesis puts non-trivial constraints on possible SN fluxes. Chakraborty, Choubey, Goswami and Kar arXiv: arXiv:0911.1218

32. Back-up Slide 2: Non-Standard effects Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 6 - 13 March 2010 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