Sébastien GALAIS S. Galais, J. Kneller, C. Volpe and J. Gava
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Transcript of Sébastien GALAIS S. Galais, J. Kneller, C. Volpe and J. Gava
The shockwave impact upon the Diffuse Supernova Neutrino
Background
GDR Neutrino, Ecole Polytechnique
Sébastien GALAIS
S. Galais, J. Kneller, C. Volpe and J. GavaPhys.Rev.D81:053002,2010 / arxiv:0906.5294 [hep-ph]
Plan
Diffuse Supernova Neutrino Background (DSNB) Motivations
o Introduction
The neutrino self-interaction The shockwave effects in supernova
o Theoretical Framework
on the fluxes on the events rates
o Results
o Simplified model to reproduce the shockwave effects
Introduction
Introduction Theoretical Framework Results Simplified Model Conclusions
neutrinos
NeutronStar
1. The interaction : neutrinos interact each other giving rise to collective effects.
- J. T. Pantaleone, Phys. Rev. D 46 510 (1992).- S. Samuel, Phys. Rev. 48, 1462 (1993).- G. Sigl and G. G. Raffelt, Nucl. Phys. B 406 423 (1993).- Y. Z. Qian and G. M. Fuller, Phys. Rev. D 51 1479 (1995).- H. Duan, G. M. Fuller, J. Carlson, and Y.-Z. Qian, Phys. Rev. 74, 105014 (2006), 0606616,…
Neutrino-sphere
Core-collapse supernova explosion
99 % of the energy is released by (anti)neutrinos of all flavors (about 1053 ergs for about 10 seconds).
Introduction
neutrinos
NeutronStar
matter
2. The shockwave effects : The shock will modify the density profile and therefore the MSW resonance.
- R. C. Schirato and G. M. Fuller (2002), 0205390.- C. Lunardini and A. Y. Smirnov, JCAP 0306, 009 (2003), 0302033.- G. L. Fogli, E. Lisi, A. Mirizzi, and D. Montanino, Phys. Rev. 68, 033005 (2003), 0304056.- J. P. Kneller, G. C. McLaughlin, and J. Brockman, Phys. Rev. 77, 045023 (2008), 0705.3835.- …
Neutrino-sphere
MSW
Introduction Theoretical Framework Results Simplified Model Conclusions
Diffuse Supernova Neutrino Background (DSNB)
Supernova explosion
Neutrinos are emitted with a Fermi-Dirac distribution:
• from a localized region.
• during a finite time.
Introduction Theoretical Framework Results Simplified Model Conclusions
Neutrinos are emitted with a Fermi-Dirac distribution:
• from all directions (past and invisible SN).
• the background is there.
DSNB
Energies are redshifted due the distance between the SN and Earth:
Much progress have been done on its ingredients such as star formation rate. - S. Ando and K. Sato, New Journal of Physics 6, 170 (2004), 0410061- L. E. Strigari, J. F. Beacom, T. P. Walker and P. Zhang, JCAP 0504, 017 (2005), 0502150- C. Lunardini, Astroparticle Physics 26, 190 (2006), 0509233- H. Yüksel and J. F. Beacom, Phys. Rev. 76, 083007 (2007), 0702613)- …
Introduction Theoretical Framework Results Simplified Model Conclusions
Motivations Numerical simulations are close to the upper limits for relic neutrinos fluxes (Super Kamiokande, LSD).
Detection window for relic neutrinos.
Introduction Theoretical Framework Results Simplified Model Conclusions
Future observatories should be able to observe these fluxes.
• MEMPHYS: 440 kTon Water Čerenkov detector.Main detection channel:
• GLACIER: 100 kTon liquid argon detector.Main detection channel:
Our aim is to explore:1)the shockwave effects (in the supernova) upon the DSNB.
2)the sensitivity to the oscillations parameters (Hierarchy, 13, phase).
• LENA: 44 kTon scintillator detector.Main detection channel:
Introduction Theoretical Framework Results Simplified Model Conclusions
• z: redshift• : energy of the neutrino at emission (neutrinosphere)• RSN: core-collapse supernova rate per unit comoving volume• : differential spectra emitted by the supernova
Theoretical framework
Diffuse Supernova Neutrino Background (DSNB) flux at Earth.
Flat universe and ΛCDM model:
ΩΛ=0.7 Ωm=0.3 H0=70 km s-1 Mpc-1
Introduction Theoretical Framework Results Simplified Model Conclusions
Supernova Rate RSN. Many constraints (Gamma-ray bursts, rest-frame UV, NIR Hα, and
FIR/sub-millimeters observations)
Star Formation Rate (RSF)
Star formation rate RSF from [1], where RSF is divided in three parts.
[1] H. Yuksel, M. D. Kistler, J. F. Beacom, and A. M. Hopkins, Astrophys. J. 683, L5 (2008).
with
Introduction Theoretical Framework Results Simplified Model Conclusions
The propagation in supernovae
e
e-
NeutronStar
MSW effect interaction Vacuum osc
Introduction Theoretical Framework Results Simplified Model Conclusions
The propagation in supernovae
e
e-
NeutronStar
MSW effect interaction Vacuum osc
Hierarchy13
Introduction Theoretical Framework Results Simplified Model Conclusions
The propagation in supernovae
e
e-
NeutronStar
MSW effect interaction Vacuum osc
SHOCK
Hierarchy13
Introduction Theoretical Framework Results Simplified Model Conclusions
Our simulationWe use a 3 flavour code in which we solve the propagation of the amplitudes. We include the interaction (single angle approximation).
J. Gava, C. Volpe, Phys.Rev.D78:083007(2008), 0807.3418.
Inverted hierarchy; 13=9, 23=40
Movies realized by S. Galais.
Introduction Theoretical Framework Results Simplified Model Conclusions
Synchronized regionBipolar oscillations
Spectral split region
Inverted hierarchy; 13=9, 23=40
Our simulation
J. Gava, C. Volpe, Phys.Rev.D78:083007(2008), 0807.3418. Movies realized by S. Galais.
Introduction Theoretical Framework Results Simplified Model Conclusions
Inverted hierarchy; 13=9, 23=40
Our simulation
J. Gava, C. Volpe, Phys.Rev.D78:083007(2008), 0807.3418. Movies realized by S. Galais.
Introduction Theoretical Framework Results Simplified Model Conclusions
Inverted hierarchy; 13=9, 23=40
Synchronized regionBipolar oscillations
Spectral split region
Our simulation
J. Gava, C. Volpe, Phys.Rev.D78:083007(2008), 0807.3418. Movies realized by S. Galais.
Introduction Theoretical Framework Results Simplified Model Conclusions
Shockwave effects in supernovae
E=20 MeV
Evolution of the density profile with time in the MSW region.
1. Before the shock (adiabatic propagation).
Without .
Impact on the probability.
Introduction Theoretical Framework Results Simplified Model Conclusions
E=20 MeV
2. The shock arrives (non-adiabatic prop.).
Without .
Shockwave effects in supernovae
Evolution of the density profile with time in the MSW region.
1. Before the shock (adiabatic propagation).
Impact on the probability.
Introduction Theoretical Framework Results Simplified Model Conclusions
E=20 MeV
3. Phase effects appear.
Without .
Shockwave effects in supernovae
2. The shock arrives (non-adiabatic prop.).
Evolution of the density profile with time in the MSW region.
1. Before the shock (adiabatic propagation).
Impact on the probability.
Introduction Theoretical Framework Results Simplified Model Conclusions
Without .
E=20 MeV
4. Post-shock propagation.
Shockwave effects in supernovae
3. Phase effects appear.
2. The shock arrives (non-adiabatic prop.).
Evolution of the density profile with time in the MSW region.
1. Before the shock (adiabatic propagation).
Impact on the probability.
Introduction Theoretical Framework Results Simplified Model Conclusions
A complete calculation including the shockwave has been realized.
Now we’re aiming at: seeing its impacts on the fluxes and events rates.
exploring the sensitivity to oscillations parameters: 13, hierarchy.
Normal Hierarchy for .
Inverted Hierarchy for .
+ shock (numerical).
RESULTS: relic electron (anti-)neutrino fluxes
For 13 we have two cases: L and S.
+ no shock (analytical).13 Small.
Results for 13 large are valid for the range:
(Me
V-1 c
m-2 s
-1)
13 Small. + no shock. + shock.
(Me
V-1 c
m-2 s
-1)
Chooz limit Best limit for future facilities
exp window
(argon detector)
exp window
(Čerenkov detector)
Normal Hierarchy for .
Inverted Hierarchy for .
Introduction Theoretical Framework Results Simplified Model Conclusions
+ shock. + no shock.
Here is plotted the ratio
Shockwave impacts:
• 10-20% effect from numerical calculations.
+ no shock. + shock.NH IH
Introduction Theoretical Framework Results Simplified Model Conclusions
+ shock. + no shock.
Here is plotted the ratio
Shockwave impacts:
• 10-20% effect from numerical calculations.
+ no shock. + shock.NH IH
• reduction of the sensitivity to 13.
Introduction Theoretical Framework Results Simplified Model Conclusions
Water Čerenkov, scintillator detectors and Inverted Hierarchy (with )
Analytical (no shock) Numerical (shock)
Nevents Detection window L L
19.3-30 MeV 0.066 0.078
Argon detectors and Normal Hierarchy
17.5-41.5 MeV 0.074 0.066
DSNB event rates (per kTon per year)
+18%
-11%
• 10-20% variation only due to the presence of the shock.
Introduction Theoretical Framework Results Simplified Model Conclusions
Water Čerenkov, scintillator detectors
Inverted Hierarchy (with )
Nevents Detection window L (no shock) L (shock) S
19.3-30 MeV 0.066 0.078 0.089
Argon detectors and Normal Hierarchy
17.5-41.5 MeV 0.074 0.066 0.058
• The sensitivity to 13 is reduced.• 10-20% variation only due to the presence of the shock.
-12%
+14%
DSNB event rates (per kTon per year)
-26%
-28%
Introduction Theoretical Framework Results Simplified Model Conclusions
• Loss of the sensitivity to collective effects in the L case.• The sensitivity to 13 is reduced.• 10-20% variation only due to the presence of the shock.
Water Čerenkov, scintillator detectors
Inverted Hierarchy (with shock)
Nevents Detection window L (with ) L (without )
19.3-30 MeV 0.078 0.078
9.3-25 MeV 0.211 0.210
+0%
+0%
DSNB event rates (per kTon per year)
Introduction Theoretical Framework Results Simplified Model Conclusions
What have we learnt?
one should include the shockwave in future simulations because its effects are significant.
To do so, we propose a simplified model to account for these effects.
1. From the numerical evolution of , we extract the 3 times.
ts: shock arrives
tp: phase effects
t∞: post-shock
2. We average the value of in each part because is independent of the energy.
A simplified model to account for the shockwave
This model based upon the general behaviour of the shockwave in supernova to calculate the flux.
Introduction Theoretical Framework Results Simplified Model Conclusions
1. From the numerical evolution of , we extract the 3 times.
ts: shock arrives
tp: phase effects
t∞: post-shock
2. We average the value of in each part because is independent of the energy.
A simplified model to account for the shockwave
This model based upon the general behaviour of the shockwave in supernova to calculate the flux.
Introduction Theoretical Framework Results Simplified Model Conclusions
Survival probability evolution with times and energy.
A simplified model to account for the shockwave Introduction Theoretical Framework Results Simplified Model Conclusions
Interval 0→ts ts→tp tp→t t→
With 0.5436 0.0634 0.3092 0.2548
Without 0.1611 0.6356 0.3531 0.4835
Times fitting with polynomials functions.
The simulations using these functions reproduce the full calculation to less than 2%.
Introduction Theoretical Framework Results Simplified Model Conclusions
Conclusions First complete calculation with interaction and shockwave for relic supernova neutrinos.
The shock affects significantly the DSNB fluxes and event rates.
We propose a model that can be used in future calculations to include shockwave effects.
S. Galais, J. Kneller, C. Volpe and J. Gava, Phys.Rev.D81:053002,2010 / arxiv:0906.5294 [hep-ph]
Introduction Theoretical Framework Results Simplified Model Conclusions
Our predictions for future observatories after 10 years
MEMPHYS, UNO
440 kTon290 < Nevents < 392
LENA
50 kTon84 < Nevents < 96
GLACIER
100 kTon58 < Nevents < 66
IH
NH
S. Galais, J. Kneller, C. Volpe and J. Gava, Phys.Rev.D81:053002,2010 / arxiv:0906.5294 [hep-ph]
Simplified model VS Numerical calculation
Here is plotted the ratio
Modification of the parameters
Variation of the cooling time .
Addition of a temporal offset t to ti.
Luminosity decreases like:
Change the arrival time of the shock.
Results are robust to variations of the cooling time and the arrival time.
Introduction DSNB Motivations Theoretical Framework Results Simplified Model Conclusions
interaction as a pendulum
S. Hannestad, G. G. Raffelt, G. Sigl, and Y. Y. Y. Wong, Phys. Rev. 74, 105010 (2006), 0608695.
Inverted Hierarchy: with without
Nevents Detection window L S
19.3-30 MeV 0.078 (0.078) 0.089 (0.066)
9.3-25 MeV 0.211 (0.210) 0.224 (0.196)
Normal Hierarchy
Detection window L or S
19.3-30 MeV 0.066
9.3-25 MeV 0.196
Inverted Hierarchy: with without
Nevents Detection window L or S
17.5-41.5 MeV 0.059 (0.058)
4.5-41.5 MeV 0.099 (0.096)
Normal Hierarchy
Detection window L S
17.5-41.5 MeV 0.066 0.058
4.5-41.5 MeV 0.106 0.096
A simplified model to account for the shockwave
SHOCK
NO SHOCK
A simplified model to account for the shockwaveNO SHOCK
Nevents(without ) > Nevents(with )
A simplified model to account for the shockwaveSHOCK
A simplified model to account for the shockwaveSHOCK
Nevents(with ) increasesNevents(without ) decreases
Nevents(with ) Nevents(without )
Interval 0→ts ts→tp tp→t t→
With 0.5436 0.0634 0.3092 0.2548
Without 0.1611 0.6356 0.3531 0.4835
Times a0 a1 a2 a3 a4 a5
ts 1.02 10-2 1.72 10-1 -6.88 10-3 1.4 10-4 -1.2 10-6 4.2 10-9
tp 9.83 10-2 1.39 10-1 -2.47 10-3 4 10-5 -4.4 10-7 1.9 10-9
t 3.75 9.5 10-2 -5 10-4
This model can be used in future calculations of DSNB fluxes and rates to include shockwave effects.
Survival probability evolution with times and energy.
Introduction DSNB Motivations Theoretical Framework Results Simplified Model Conclusions
A simplified model to account for the shockwave
Evolution of times with energy.
Introduction DSNB Motivations Theoretical Framework Results Simplified Model Conclusions
BUT the luminosity decreasesSo we must do :
A simplified model to account for the shockwave
AND
AND
1. The interaction.
- J. T. Pantaleone, Phys. Rev. D 46 510 (1992).- S. Samuel, Phys. Rev. 48, 1462 (1993).- G. Sigl and G. G. Raffelt, Nucl. Phys. B 406 423 (1993).- Y. Z. Qian and G. M. Fuller, Phys. Rev. D 51 1479 (1995).- S. Pastor, G. G. Raffelt, and D. V. Semikoz, Phys. Rev. 65, 053011 (2002), 0109035.- H. Duan, G. M. Fuller, J. Carlson, and Y.-Z. Qian, Phys. Rev. 74, 105014 (2006), 0606616.- S. Hannestad, G. G. Raffelt, G. Sigl, and Y. Y. Y. Wong, Phys. Rev. 74, 105010 (2006), 0608695.- A. B. Balantekin and Y. Pehlivan, J. Phys. 34, 47 (2007), 0607527.- G. G. Raffelt and A. Y. Smirnov, Phys. Rev. 76, 125008 (2007), 0709.4641.- …
Recent developments in neutrino propagation in SN:
After the explosion of the star, the neutrinos density is so high that neutrinos interact each other giving rise to collective effects like synchronization, bipolar oscillations and spectral split.
Introduction
2. The shockwave effects.
- R. C. Schirato and G. M. Fuller (2002), 0205390.- C. Lunardini and A. Y. Smirnov, JCAP 0306, 009 (2003), 0302033.- K. Takahashi, K. Sato, H. E. Dalhed, and J. R. Wilson, Astropart. Phys. 20, 189 (2003), 0212195.- G. L. Fogli, E. Lisi, A. Mirizzi, and D. Montanino, Phys. Rev. 68, 033005 (2003), 0304056.- R. Tomas, M. Kachelrieß, G. Raffelt, A. Dighe, H.-T. Janka, and L. Scheck, JCAP 0409, 015 (2004), 0407132.- G. L. Fogli, E. Lisi, A. Mirizzi, and D. Montanino, JCAP 4, 2 (2005), 0412046.- S. Choubey, N. P. Harries, and G. G. Ross, Phys. Rev. D74, 053010 (2006), 0605255.- B. Dasgupta and A. Dighe, Phys. Rev. 75, 093002 (2007), 0510219.- S. Choubey, N. P. Harries, and G. G. Ross, Phys. Rev. 76, 073013 (2007), 0703092.- J. P. Kneller, G. C. McLaughlin, and J. Brockman, Phys. Rev. 77, 045023 (2008), 0705.3835.- J. P. Kneller and G. C. McLaughlin, Phys. Rev. 73, 056003 (2006), 0509356.- …
Introduction
The shock propagates through the matter in which it will modify the density profile and therefore the MSW resonance.
Introduction DSNB Motivations Theoretical Framework Results Conclusions
- …- I.K. Baldry and K. Glazebrook, Astrophys. J. 593, 258 (2003).- S. Ando and K. Sato, New Journal of Physics 6, 170 (2004), 0410061.- L. E. Strigari, J. F. Beacom, T. P. Walker and P. Zhang, JCAP 0504, 017 (2005), 0502150. - C. Lunardini, Astroparticle Physics 26, 190 (2006), 0509233.- H. Yüksel and J. F. Beacom, Phys. Rev. 76, 083007 (2007), 0702613.- S. Chakraborty, S. Choubey, B. Dasgupta, and K. Kar, JCAP 0809, 013 (2008), 08053131.- …
3. Progress on the Diffuse Supernova Neutrino Background (DSNB).
Introduction
There have been much progress on the ingredients of the DSNB such as star formation rate, initial mass function.
Normal Hierarchy Analytic (no shock) Numeric (shock)
Nevents Detection window L L
17.5-41.5 MeV 0.074 0.066
4.5-41.5 MeV 0.116 0.106
Argon detectors.
Inverted Hierarchy: with Analytic (no shock) Numeric (shock)
Nevents Detection window L L
19.3-30 MeV 0.066 0.078
9.3-25 MeV 0.196 0.211
Water Cerenkov and scintillator detectors. per kTon per year
DSNB event rates in -observatories
+18%
+8%
- 9%
-11%
• 10% variation only due to the presence of the shock.
Inverted Hierarchy: with + shock
Nevents Detection window L S
19.3-30 MeV 0.078 0.089
9.3-25 MeV 0.211 0.224
Normal Hierarchy
Nevents Detection window L S
17.5-41.5 MeV 0.066 0.058
4.5-41.5 MeV 0.106 0.096
Argon detectors.
per kTon per year
DSNB event rates in -observatories
Water Cerenkov and scintillator detectors.
+14%
- 6%
-12%
• Same variation due to 13.• 10% variation only due to the presence of the shock.
Inverted Hierarchy: with + shock
Nevents Detection window L (with L (without
19.3-30 MeV 0.078 0.078
9.3-25 MeV 0.211 0.210
Normal Hierarchy
Nevents Detection window L
17.5-41.5 MeV 0.066
4.5-41.5 MeV 0.106
Argon detectors.
per kTon per year
DSNB event rates in -observatories
Water Cerenkov and scintillator detectors.
• Loss of the sensitivity to collective effects in the L case.• Same variation due to 13.
+0%
+0%
• 10% variation only due to the presence of the shock.
The method usedWe use a 3 flavour code in which we solve the propagation of the amplitudes. We include the interaction (single angle approximation).
J. Gava, C. Volpe, Phys.Rev.D78:083007(2008), 0807.3418.
3. Spectral split.
This gives our at the supernova.
interactionInverted Hierarchy.
1. Synchronized region.
2. Bipolar oscillations.
MSW effect
DSNB Motivations Theoretical Framework Results Conclusions