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

Outline Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 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

Neutrino Production in Supernovae

SN Explosion and Neutrino Emission Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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  K T  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

SN Explosion and Neutrino Emission Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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  g cm -3 T  30 MeV Neutrino Cooling

Neutrino Luminosities and Energies Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Luminosity in 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/

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

Neutrino Propagation and Flavor Conversions Neutrino Propagation and Flavor Conversions

Free-Streaming Neutrinos Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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 

Lot of activity in recent years Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Seminal papers: Duan, Fuller, Carlson and Qian in 2005, 2006 Pendulum Analogy: Hannestad, Raffelt, Sigl and Wong, arXiv:astro-ph/ 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 …

Collective Flavor Conversion Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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

Collective Flavor Conversion Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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

Spectral Swaps/Splits Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Dasgupta, Dighe, Raffelt and Smirnov, arXiv: (PRL) For movies see

Spectral Swaps/Splits Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Dasgupta, Dighe, Raffelt and Smirnov, arXiv: (PRL) For movies see

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

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

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

MSW conversions in SN Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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/

Regeneration in Earth Matter Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Electron flavor flux = cos 2  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!

Neutrino Detection

Running (soon) SN Neutrino Detectors Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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

Main Detection Channels Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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.

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, March 2010 e can be identified by delayed coincidence. e can be identified by delayed coincidence. n+Gd → ~8 MeV  (90%) n+p → d MeV  (10%) Beacom and Vagins, arXiv:hep-ph/ (PRL) Can identify each antineutrino on an event-by-event basis Gadolinium Anti-nu Detector Zealously Outperforming Old Kamiokande. Super!

What Can We Learn ?

SN pointing alerts/SNEWS Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Beacom and Vogel, arXiv: astro-ph/ Tomas, Semikoz, Kachelriess, Raffelt and Dighe, arXiv: hep-ph/ 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

Stellar Explosion Dynamics Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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)

Diffuse Neutrino Background Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Estimated present-day flux from all SN in our past~ 10 cm -2 s -1 Beacom and Vagins, hep-ph/ (PRL) Horiuchi, Beacom and Dwek, arXiv: Guaranteed source of neutrinos from cosmological distances See also Chakraborty, Choubey, Dasgupta and Kar, arXiv: for effect of collective oscillations on DSNB for effect of collective oscillations on DSNB

 13 Estimate/Shockwave effects Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 2010 Tomas, Kachelriess, Dighe, Raffelt and Janka, arXiv:astro-ph/ Most of the work on this was done around Needs to be re-done after including collective effects e.g. Gava, Kneller, Volpe and Mc Laughlin, arXiv: (PRL)

Neutrino Mass Hierarchy Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, 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: (PRL)

Summary Basudeb Dasgupta, Rencontres de Moriond - Electroweak Session-2010 at La Thuile, Italy, March 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

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

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