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Neutrinos from Supernovae International Conference in High Energy - - PowerPoint PPT Presentation

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Basudeb Dasgupta Neutrinos from Supernovae International Conference in High Energy Physics ICHEP 2010, 22-28 July 2010, Paris, France Menu du jour www.ps.uci.edu/~tomba/sk/tscan Neutrino Neutrino Propagation and Neutrino Production Flavor

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SLIDE 1

Neutrinos from Supernovae

Basudeb Dasgupta International Conference in High Energy Physics ICHEP 2010, 22-28 July 2010, Paris, France

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SLIDE 2

Menu du jour

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

www.ps.uci.edu/~tomba/sk/tscan

Neutrino Production Neutrino Detection Neutrino Propagation and Flavor Conversion Neutrino Astronomy Supernova Astrophysics Neutrino properties and particle physics

  • 1. Pointing in advance/SN alerts
  • 2. Signatures of stellar dynamics
  • 3. Tracking the local SN rate
  • 4. Timing/GW-coincidence
  • 1. Neutrino Mass Hierarchy

2.

13 estimate

  • 3. QCD phase transition
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SLIDE 3

Neutrino Production in Supernovae

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SLIDE 4

SN Explosion and Neutrino Emission

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Main-sequence star Hydrogen gen Burning ing Helium-burning star Heliu ium Burni ning Hydrogen gen Burni ning ng Onion structure

Degenerate iron core: 109 g cm-3 T 1010 K MFe 1.5 Msun RFe 8000 km

Collapse (implosion)

Adapted from a slide by Georg Raffelt

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SLIDE 5

SN Explosion and Neutrino Emission

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Collapse (implosion) Bounce (explosion)

e Burst

Prompt Shock Stalls Neutrino Heating Neutrino Driven Explosion Newborn Neutron Star ~ 50 km

Proto-Neutron Star

nuc = 3

1014 g cm-3 T 30 MeV

Neutrino Cooling

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SLIDE 6

Neutrino Luminosities and Energies

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Luminosity in 1051erg/s For e, anti- e and x Average Energy in MeV For e, anti- e and x

Raffelt, Keil, Buras, Janka and Rampp, arXiv:astro-ph/0303226

Accretion Phase Cooling Phase Burst Phase

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SLIDE 7

Neutrino Propagation and Flavor Conversions

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SLIDE 8

Free-Streaming Neutrinos

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

] ), )[( cos 1 ( 2 q d G 2 ] , L [ G 2 , p 2 M i

p q q q p 3 3 F p F p 2 p t        

MSW effect depends on

  • rdinary matter density L,

i.e. mainly e density

Vacuum oscillations

  • M is neutrino mass matrix
  • minus sign for antineutrinos

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

Talk by Antonio Marrone, ICHEP-2010

Pantaleone Mikheev, Smirnov, Wolfenstein Pontecorvo

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SLIDE 9

Status Report at ICHEP 2008

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Neutrinos Plenary Talk by Zhi-Zhong Xing, ICHEP-2008

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SLIDE 10

Spectral Swaps: Accretion Phase

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Fogli, Lisi, Marrone and Mirizzi, arXiv: 0707.1998

Nontrivial Evolution only for Inverted Hierarchy

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SLIDE 11

Collective Flavor Conversion

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Swap cannot be complete, because of Total Lepton Number Conservation

Instability in Flavor Space  Swap around spectral crossings Flavor Fluxes Energy Energy

e e

Initial Final

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SLIDE 12

Spectral Swaps: Cooling Phase

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Dasgupta, Dighe, Raffelt and Smirnov, arXiv: 0904.3542 (PRL)

Spectral Splits in Inverted Hierarchy Spectral Splits in Normal Hierarchy

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SLIDE 13

3 Flavor Spectral Swaps: Cooling Phase

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Friedland, arXiv:1001.0996 (PRL) Dasgupta, Mirizzi, Tamborra and Tomas, arXiv:1002.2943

NH IH

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SLIDE 14

Late-time + Angle-dependent + 3 flavors

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Duan and Friedland, arXiv: 1006.2359

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SLIDE 15

Survey of Flux Models

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Fogli, Lisi, Marrone and Tamborra, arXiv:0907.5115 Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx

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SLIDE 16

MSW conversions in SN

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

NH IH Spectral Splits in Inverted Hierarchy L resonance : 1

2

( mso

sol 2 ,

, 12

12)

) at 101 – 102 g/cc

Always in neutrinos. Always adiabatic.

Spectral Splits in H resonance : 1/ 2

3

( matm

atm 2 ,

, 13

13)

) at 103 – 104 g/cc In neutrinos for NH and in antineutrinos for IH. Adiabaticity ≈ sin2

13

Dighe and Smirnov, arXiv: hep-ph/9907423

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SLIDE 17

Regeneration in Earth Matter

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Electron flavor flux = cos2

12 1 + sin2 12 2

Electron flavor: = (1-P2e) 1 + P2e 2 P2e is the probability of 2 to

e

which depends on Earth density and L

L Detector Location Matters!

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SLIDE 18

Survival Probabilities

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  • B. Dasgupta, arXiv:hep-ph/1005.2681 [Moriond-2010, Proceedings]

<

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SLIDE 19

Neutrino Detection

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SLIDE 20

Running (soon) SN Neutrino Detectors

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Hyper-K/UNO/MEMPHYS/LENA/Km3NET/… Icecube Super-K KamLAND Mini-BOONE LVD Borexino Baksan Icarus HALO SNO+ NO A ✔ ✔ ✔ ✔=Large (>103 events for 10kpc SN) Daya-Bay

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SLIDE 21

Main Detection Channels

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

  • SK-like water Cherenkov detector (30 kt, SN at 10kpc)
  • Scintillation detector
  • Liquid Argon detector

Liquid Argon TPC can see neutrinos,

  • thers mostly see

antineutrinos Super-Kamiokande and Icecube are at present our largest detectors for SN neutrinos.

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SLIDE 22

Positron and gamma ray vertices are within ~50cm.

[reaction schematic by M. Nakahata]

e

e+

p n

p Gd Gadzooks

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

e can

n be id ident ntifi ified ed by y delaye yed d coinciden incidence. e. 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!
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SLIDE 23

What Can We Learn ?

  • Astrophysics -
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SLIDE 24

SN pointing alerts/SNEWS

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 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! SNEWS http://snews.bnl.gov

Coincidence at multiple detectors will trigger an alert for astronomers

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SLIDE 25

Stellar Explosion Dynamics

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

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 and Raffelt: astro-ph/1006.1889

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SLIDE 26

Diffuse Neutrino Background

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Estimated present-day flux from all SN in our past~ 10 cm-2 s-1

e

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

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SLIDE 27

Coincidence with Gravity Wave Expts

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

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

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SLIDE 28

What Can We Learn ?

  • Particle Physics -
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SLIDE 29

Can we see the splits? Perhaps…for Cooling.

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx

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SLIDE 30

Accretion phase signals…a bit weaker.

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx

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SLIDE 31

Earth Matter Effects

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Choubey, Dasgupta, Dighe and Mirizzi, arXiv:1008.xxxx 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.

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SLIDE 32

Neutrino Mass Hierarchy

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 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)

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SLIDE 33

13 Estimate/Shockwave effects

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

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)

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SLIDE 34

QCD anti-nu burst detectable from SN

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

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

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SLIDE 35

Summary

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

www.ps.uci.edu/~tomba/sk/tscan

Neutrino Production Neutrino Detection Neutrino Propagation and Flavor Conversion Neutrino Astronomy Supernova Astrophysics Neutrino properties and particle physics

  • 1. Pointing in advance/SN alerts
  • 2. Signatures of stellar dynamics
  • 3. Tracking the local SN rate
  • 4. Timing/GW-coincidence
  • 5. …
  • 1. Neutrino Mass Hierarchy

2.

13 estimate

  • 3. QCD phase transition
  • 4. …
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SLIDE 36

Back-up Slide 1: R-process nucleosynthesis

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 2010

Demanding successful R-process nucleosynthesis puts non-trivial constraints on possible SN fluxes.

Chakraborty, Choubey, Goswami and Kar, arXiv: arXiv:0911.1218

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SLIDE 37

Back-up Slide 2: Non-Standard effects

Basudeb Dasgupta, ICHEP-2010 at Paris, France, 22 - 28 July 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