1 / 37

Menu du jour

Menu du jour. 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 properties and particle physics .

liona
Download Presentation

Menu du jour

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Menu du jour 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 properties and particle physics Pointing in advance/SN alerts Signatures of stellar dynamics Tracking the local SN rate Timing/GW-coincidence Neutrino Mass Hierarchy Q13 estimate QCD phase transition Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  2. Neutrino Production in Supernovae

  3. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  4. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  5. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  6. Neutrino Propagation and Flavor Conversions

  7. 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 • minus sign for antineutrinos MSW effect depends on ordinary matter density L, i.e. mainly e density Nonlinear Effects depends on the neutrino density r Pontecorvo Mikheev, Smirnov,Wolfenstein Pantaleone Talk by Antonio Marrone, ICHEP-2010 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  8. Status Report at ICHEP 2008 Neutrinos PlenaryTalk by Zhi-Zhong Xing, ICHEP-2008 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  9. Spectral Swaps: Accretion Phase Nontrivial Evolution only for Inverted Hierarchy Fogli, Lisi, Marrone and Mirizzi, arXiv: 0707.1998 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  10. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  11. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  12. 3 Flavor Spectral Swaps: Cooling Phase NH IH Friedland, arXiv:1001.0996 (PRL) Dasgupta, Mirizzi, Tamborra and Tomas, arXiv:1002.2943 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  13. Late-time + Angle-dependent + 3 flavors Duan and Friedland, arXiv: 1006.2359 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  14. Survey of Flux Models Fogli, Lisi, Marrone and Tamborra, arXiv:0907.5115 Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  15. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  16. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  17. Survival Probabilities < B. Dasgupta, arXiv:hep-ph/1005.2681 [Moriond-2010, Proceedings] Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  18. Neutrino Detection

  19. Running (soon) SN Neutrino Detectors SNO+ Baksan HALO Icarus ✔ Mini-BOONE Daya-Bay Super-K LVD Borexino KamLAND ✔ NOnA ✔ Icecube Hyper-K/UNO/MEMPHYS/LENA/Km3NET/… ✔=Large (>103 events for 10kpc SN) Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  20. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  21. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  22. What Can We Learn ? - Astrophysics -

  23. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  24. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  25. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  26. Coincidence with Gravity Wave Expts SN neutrino-curve is an excellent probe of the bounce time. This can be used to great advantage for coincidence measurement with gravitational wave detectors Pagliaroni, Vissani, Coccia and Fulgione, arXiv:0903:1191 (PRL) Halzen and Raffelt, arXiv:0908.2317 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  27. What Can We Learn ? - Particle Physics -

  28. Can we see the splits? Perhaps…for Cooling. Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  29. Accretion phase signals…a bit weaker. Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  30. Earth Matter Effects Ratio of events between shadowed and unshadowed WC detectors is an excellent probe of the Neutrino Mass Hierarchy Fourier analysis of the event rate reveals earth effect oscillations for a single Liq. Argon/Scintillator detector. Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  31. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  32. Q13Estimate/Shockwave effects Tomas, Kachelriess, Dighe, Raffelt and Janka, arXiv:astro-ph/0407132 Most of the work on this was done around 2000-2004 After including collective effects … e.g. Gava, Kneller, Volpe and Mc Laughlin, arXiv:0902.0317 (PRL) Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  33. QCD anti-nu burst detectable from SN Sagert, Fischer, Hempel, Pagliara, Schaffner-Bielich, Mezzacappa, Thielemann, and Liebendoerfer, arXiv:0809.4225 (PRL) Dasgupta, Fischer, Horiuchi, Liebendorfer, Mirizzi, Sagert and Schaffner-Bielich arXiv:0912.2568 2nd Shock Break-out Width = ~5ms Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  34. 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 properties and particle physics Pointing in advance/SN alerts Signatures of stellar dynamics Tracking the local SN rate Timing/GW-coincidence … Neutrino Mass Hierarchy Q13 estimate QCD phase transition … Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  35. Back-up Slide 1: R-process nucleosynthesis Demanding successful R-process nucleosynthesis puts non-trivial constraints on possible SN fluxes. Chakraborty, Choubey, Goswami and Kar, arXiv: arXiv:0911.1218 Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  36. 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, ICHEP-2010 at Paris, France, 22 - 28 July 2010

More Related