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High energy neutrinos from astrophysical sources:a self-consistent approach
Ricard Tomàs
AHEP Group - Institut de Física Corpuscular(CSIC - Universitat de València)
based on Phys. Rev. D 74 (2006) 063009 [astro-ph/0606406]
in collaboration with M. Kachelrieß
JIGSAW 2007Joint Indo-German School And Workshop 2007
Neutrinos in Physics, Astrophysics and Cosmology19 February 2007 - Mumbai, India
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 1 / 34
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 2 / 34
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 2 / 34
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 2 / 34
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 2 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomy
interior of stars [G. G. Raffelt, 1996, R. C. Schirato and G. M. Fuller, 2002]
distant cosmological epochs→ relic neutrino absorption spectroscopy[B. Eberle, A. Ringwald, L. Song and T. Weiler, 2004]
origin of UHECRs→ characterize astrophysical sources[L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, 2005, T. Kashti and E. Waxman, 2005,
M. Ahlers, L. A. Anchordoqui, H. Goldberg, F. Halzen, A. Ringwald, and Th. J. Weiler, 2005]
ν conversion from the source to the detector →
Main problem: low statistics
Requirements: ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavouredSHDM : disfavoured
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomyν conversion from the source to the detector → ν properties
mixing angles [H. Athar, M. Jezabek and O. Yasuda, 2000, P. Bhattacharjee and N. Gupta, 2005,
P. D. Serpico and M. Kachelrieß, 2005, M. C. González-García, F. Halzen and M. Maltoni, 2005, P. Serpico, 2005]
CP phase [P. D. Serpico and M. Kachelrieß, 2005, W. Rodejohann, 2007]
ν decay [J. F. Beacom et al, 2002, G. Barenboim and C. Quigg, 2003, D. Meloni and T. Ohlsson, 2006]
+ terrestrial experiments→mass hierarchy [W. Winter, 2006]
Main problem: low statistics
Requirements: ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavouredSHDM : disfavoured
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomyν conversion from the source to the detector → ν properties
Main problem: low statistics
Requirements: ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavouredSHDM : disfavoured
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomyν conversion from the source to the detector → ν properties
Main problem: low statistics
Requirementsbig ν detection volume : ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavouredSHDM : disfavoured
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomyν conversion from the source to the detector → ν properties
Main problem: low statistics
Requirementsbig ν detection volume : ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavoured by EGRET and spectral shape of UHECRsSHDM : disfavoured by the absence of γ at high energies and galactic anisotropy
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Motivation
Motivation
Interest of high energy neutrinos (HE ν)penetrating power + no deflection → neutrino astronomyν conversion from the source to the detector → ν properties
Main problem: low statistics
Requirementsbig ν detection volume : ICECUBE, Auger, Anita, ...
flavor determination[D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003]
large HE ν fluxestop-down models:
topological defects: disfavouredSHDM : disfavoured
bottom-up models→ astrophysical sources→ optically thick
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 3 / 34
Astrophysical sources
Astrophysical sources
Limits
[P. Lipari, 2006]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 4 / 34
Astrophysical sources
Astrophysical sources
LimitsWaxman-Bahcall upper limit on high energy ν fluxes [E. Waxman and J. N. Bahcall, 1999]
−→ E2φν(E) . 10−8 GeV/cm2s sr
only applies to optically thin sources↓
is it possible to get large HEν fluxes from optically thick sources?do they have any special feature?
Result
thick (τ & 1)→ multiple scattering suppresses CR flux
not high density→ not to suppress π and K decays
strongly energy dependent flavor ratio → a bump shows up
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 5 / 34
Astrophysical sources
Astrophysical sources
LimitsWaxman-Bahcall upper limit on high energy ν fluxes [E. Waxman and J. N. Bahcall, 1999]
−→ E2φν(E) . 10−8 GeV/cm2s sr
only applies to optically thin sources↓
is it possible to get large HEν fluxes from optically thick sources?do they have any special feature?
Result
thick (τ & 1)→ multiple scattering suppresses CR flux
not high density→ not to suppress π and K decays
strongly energy dependent flavor ratio → a bump shows up
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 5 / 34
Astrophysical sources
Astrophysical sources
LimitsWaxman-Bahcall upper limit on high energy ν fluxes [E. Waxman and J. N. Bahcall, 1999]
−→ E2φν(E) . 10−8 GeV/cm2s sr
only applies to optically thin sources↓
is it possible to get large HEν fluxes from optically thick sources?do they have any special feature?
Resultlarge HEν fluxes → sources
thick (τ & 1)→ multiple scattering suppresses CR flux
not high density→ not to suppress π and K decays
strongly energy dependent flavor ratio → a bump shows up
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 5 / 34
Astrophysical sources
Astrophysical sources
LimitsWaxman-Bahcall upper limit on high energy ν fluxes [E. Waxman and J. N. Bahcall, 1999]
−→ E2φν(E) . 10−8 GeV/cm2s sr
only applies to optically thin sources↓
is it possible to get large HEν fluxes from optically thick sources?do they have any special feature?
Resultlarge HEν fluxes → sources
thick (τ & 1)→ multiple scattering suppresses CR fluxnot high density→ not to suppress π and K decays
strongly energy dependent flavor ratio → a bump shows up
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 5 / 34
Astrophysical sources
Astrophysical sources
LimitsWaxman-Bahcall upper limit on high energy ν fluxes [E. Waxman and J. N. Bahcall, 1999]
−→ E2φν(E) . 10−8 GeV/cm2s sr
only applies to optically thin sources↓
is it possible to get large HEν fluxes from optically thick sources?do they have any special feature?
Resultlarge HEν fluxes → sources
thick (τ & 1)→ multiple scattering suppresses CR fluxnot high density→ not to suppress π and K decays
strongly energy dependent flavor ratio → a bump shows up
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 5 / 34
Astrophysical sources Optically thick sources as neutrino sources
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 6 / 34
Astrophysical sources Optically thick sources as neutrino sources
Optically thick sources
Transparent sources: accelerated protons interact once with thesurrounding material → relationship ν ↔ UHECR ↔ γ’soptical depth τ ≡ L/lint < 1
↑
Optically thick sources
↓
Hidden source: source which accelerates particles to high-energies, but itis not seen in high-energy electromagnetic radiation, τ >> 1
cocooned black hole [V. S. Berezinsky and V. L Ginzburg, 1987]
cores of AGNs [F. Stecker, C. Done, M. Salamon and P. Sommers, 1991]
collapsing galactic nucleus [V. S. Berezinsky and V. I. Dokuchaev, 2001]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 7 / 34
Astrophysical sources Optically thick sources as neutrino sources
Optically thick sources
Transparent sources: accelerated protons interact once with thesurrounding material → relationship ν ↔ UHECR ↔ γ’soptical depth τ ≡ L/lint < 1
↑
Optically thick sources
↓
Hidden source: source which accelerates particles to high-energies, but itis not seen in high-energy electromagnetic radiation, τ >> 1
cocooned black hole [V. S. Berezinsky and V. L Ginzburg, 1987]
cores of AGNs [F. Stecker, C. Done, M. Salamon and P. Sommers, 1991]
collapsing galactic nucleus [V. S. Berezinsky and V. I. Dokuchaev, 2001]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 7 / 34
Astrophysical sources Optically thick sources as neutrino sources
Optically thick sources
Transparent sources: accelerated protons interact once with thesurrounding material → relationship ν ↔ UHECR ↔ γ’soptical depth τ ≡ L/lint < 1
↑
Optically thick sources
↓
Hidden source: source which accelerates particles to high-energies, but itis not seen in high-energy electromagnetic radiation, τ >> 1
cocooned black hole [V. S. Berezinsky and V. L Ginzburg, 1987]
cores of AGNs [F. Stecker, C. Done, M. Salamon and P. Sommers, 1991]
collapsing galactic nucleus [V. S. Berezinsky and V. I. Dokuchaev, 2001]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 7 / 34
Astrophysical sources Optically thick sources as neutrino sources
Optically thick sources as neutrino sources
Our Monte Carlo simulation
source: phenomenological characterizationinjected protons dN/dE ∝ E−α −→ (α = 2.2, Emax = 1024 eV)
slab with
−protons
−thermal photons −→
− size L− temperature T− magnetic field negligible
interactions: SOPHIA [A. Mücke et al., 2000] and HERWIG [G. Corcella et al., 2001]
p + γ → secondary mesons
π → µ + νµ → e + νe + νµ + νµ
K± → µ + νµ , π± + π0 , . . .K 0
L → π + e + νe , π + µ + νµ , . . .charm mesons decay
↓High Energy Neutrinos
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 8 / 34
Astrophysical sources Optically thick sources as neutrino sources
Optically thick sources as neutrino sources
Our Monte Carlo simulation
source: phenomenological characterizationinjected protons dN/dE ∝ E−α −→ (α = 2.2, Emax = 1024 eV)
slab with
−protons
−thermal photons −→
− size L− temperature T− magnetic field negligible
interactions: SOPHIA [A. Mücke et al., 2000] and HERWIG [G. Corcella et al., 2001]
p + γ → secondary mesons
π → µ + νµ → e + νe + νµ + νµ
K± → µ + νµ , π± + π0 , . . .K 0
L → π + e + νe , π + µ + νµ , . . .charm mesons decay
↓High Energy Neutrinos
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 8 / 34
Spectra from a single source Neutrino Yield
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 9 / 34
Spectra from a single source Neutrino Yield
Neutrino Yield: Yν =Jν(E)τJp(E)
[V. S. Berezinsky and V. V. Volynsky, 1979, V. S. Berezinsky and A. Z. Gazizov, 1993]
transparent source τ < 1
Yν = Yν(x) , dimensionless energy x ≡ Eωm2
p, ω = 1.6T
contribution: mainly from π decays: π → µ + νµ → e + νe + 2νµ
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 10 / 34
Spectra from a single source Neutrino Yield
contributionsmainly
π decayneutron decay
(at low energies)
T = 104 K, τ = 0.4
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 11 / 34
Spectra from a single source Neutrino Yield
Neutrino Yield: Yν =Jν(E)τJp(E)
[V. S. Berezinsky and V. V. Volynsky, 1979, V. S. Berezinsky and A. Z. Gazizov, 1993]
transparent source τ < 1
Yν = Yν(x) , dimensionless energy x ≡ Eωm2
p, ω = 1.6T
contribution: mainly from π decays: π → µ + νµ → e + νe + 2νµ
independent of T and τ
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 12 / 34
Spectra from a single source Neutrino Yield
T = 104 K T = 105 K
independent of T
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 13 / 34
Spectra from a single source Neutrino Yield
T = 104 K T = 105 K
independent of T and τ
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 13 / 34
Spectra from a single source Neutrino Yield
Neutrino Yield: Yν =Jν(E)τJp(E)
[V. S. Berezinsky and V. V. Volynsky, 1979, V. S. Berezinsky and A. Z. Gazizov, 1993]
transparent source τ < 1
Yν = Yν(x) , dimensionless energy x ≡ Eωm2
p, ω = 1.6T
contribution: mainly from π decays: π → µ + νµ → e + νe + 2νµ
independent of T and τ
optically thick sources τ & 1
multiple scattering important → critical energy xπ,Kcr (T ) : ldecay = lint
contribution depends on the energyx < xπ
cr −→ pion decayxπ
cr <∼ x <∼ xKcr → K decay
xKcr < x −→ charm meson decay
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 14 / 34
Spectra from a single source Neutrino Yield
T = 104 K, τ = 40
x < xπcr → pion decay dominates
xπcr <∼ x <∼ xK
cr → π’s scatter before decaying ⇒ K decay important
xKcr < x → K ’s scatter before decaying ⇒ charm meson decay dominates
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 15 / 34
Spectra from a single source Neutrino Yield
Neutrino Yield: Yν =Jν(E)τJp(E)
[V. S. Berezinsky and V. V. Volynsky, 1979, V. S. Berezinsky and A. Z. Gazizov, 1993]
transparent source τ < 1
Yν = Yν(x) , dimensionless energy x ≡ Eωm2
p, ω = 1.6T
contribution: mainly from π decays: π → µ + νµ → e + νe + 2νµ
independent of T and τ
optically thick sources τ & 1
multiple scattering important → critical energy xπ,Kcr (T ) : ldecay = lint
contribution depends on the energyx < xπ
cr −→ pion decayxπ
cr <∼ x <∼ xKcr → K decay
xKcr < x −→ charm meson decay
Yν depends on T : xπcr ≈ 2× 1010/(T/K)2
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 16 / 34
Spectra from a single source Neutrino Yield
T = 104 K T = 105 K
Large HE ν flux ifopaque sources (τ & 1 ⇒ L & lpint) to avoid the WB upper limitnot very high temperature (Ecr ∝ 1/T 3)
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 17 / 34
Spectra from a single source Unnormalized neutrino fluxes
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 18 / 34
Spectra from a single source Unnormalized neutrino fluxes
Unnormalized Neutrino Spectra: thickness
T = 105 K
τ & 1 =⇒ cosmic ray suppression
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 19 / 34
Spectra from a single source Unnormalized neutrino fluxes
Unnormalized Neutrino Spectra: thickness
T = 105 K
τ & 1 =⇒ cosmic ray suppression
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 19 / 34
Spectra from a single source Unnormalized neutrino fluxes
Unnormalized Neutrino Spectra: thickness
T = 105 K
τ & 1 =⇒ cosmic ray suppression
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 19 / 34
Spectra from a single source Unnormalized neutrino fluxes
Unnormalized Neutrino Spectra: thickness
T = 105 K
τ & 1 =⇒ cosmic ray suppression
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 19 / 34
Spectra from a single source Unnormalized neutrino fluxes
Unnormalized Neutrino Spectra: temperature
T = 104 K T = 107 K
high temperature =⇒ high-energy ν flux suppression
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 20 / 34
Spectra from a single source Unnormalized neutrino fluxes
Conditions for large HEν fluxes
opaque source (τ & 1) and not too dense
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 21 / 34
Spectra from a single source Flavor content
Outline
1 Motivation
2 Astrophysical sourcesOptically thick sources as neutrino sources
3 Spectra from a single sourceNeutrino YieldUnnormalized neutrino fluxesFlavor content
4 Summary
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 22 / 34
Spectra from a single source Flavor content
Flavor content (φνe, φνµ, φντ
)
Motivationmeasurable in ν telescopes and extensive air shower experiments[J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003, D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000]
: characterize sources[L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, 2005, T. Kashti and E. Waxman, 2005]
learn about [H. Athar, M. Jezabek and O. Yasuda, 2000, P. Bhattacharjee and N. Gupta, 2005,
P. D. Serpico and M. Kachelrieß, 2005, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, 2002, W. Winter, 2006]
Examplepion decay → (1,2,0)neutron beam source → (1,0,0) [L. A. Anchordoqui et al., 2003, P. D. Serpico and M. Kachelrieß, 2005]
muon-damped νµ sources from π decay → (0,1,0)[J. P. Rachen and P. Meszaros, 1998, T. Kashti and E. Waxman, 2005]
optically thick sources → (φνe , φνµ , φντ ) ?
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 23 / 34
Spectra from a single source Flavor content
Flavor content (φνe, φνµ, φντ
)
Motivationmeasurable in ν telescopes and extensive air shower experiments[J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003, D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000]
interesting applicationsastrophysical diagnostics: characterize sources[L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, 2005, T. Kashti and E. Waxman, 2005]
learn about ν properties [H. Athar, M. Jezabek and O. Yasuda, 2000, P. Bhattacharjee and N. Gupta, 2005,
P. D. Serpico and M. Kachelrieß, 2005, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, 2002, W. Winter, 2006]
Examplepion decay → (1,2,0)neutron beam source → (1,0,0) [L. A. Anchordoqui et al., 2003, P. D. Serpico and M. Kachelrieß, 2005]
muon-damped νµ sources from π decay → (0,1,0)[J. P. Rachen and P. Meszaros, 1998, T. Kashti and E. Waxman, 2005]
optically thick sources → (φνe , φνµ , φντ ) ?
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 23 / 34
Spectra from a single source Flavor content
Flavor content (φνe, φνµ, φντ
)
Motivationmeasurable in ν telescopes and extensive air shower experiments[J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003, D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000]
interesting applicationsastrophysical diagnostics: characterize sources[L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, 2005, T. Kashti and E. Waxman, 2005]
learn about ν properties [H. Athar, M. Jezabek and O. Yasuda, 2000, P. Bhattacharjee and N. Gupta, 2005,
P. D. Serpico and M. Kachelrieß, 2005, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, 2002, W. Winter, 2006]
Examplepion decay → (1,2,0)neutron beam source → (1,0,0) [L. A. Anchordoqui et al., 2003, P. D. Serpico and M. Kachelrieß, 2005]
muon-damped νµ sources from π decay → (0,1,0)[J. P. Rachen and P. Meszaros, 1998, T. Kashti and E. Waxman, 2005]
optically thick sources → (φνe , φνµ, φντ
) ?
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 23 / 34
Spectra from a single source Flavor content
Flavor content (φνe, φνµ, φντ
)
Motivationmeasurable in ν telescopes and extensive air shower experiments[J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa and T. J. Weiler, 2003, D. Fargion, 1997, S. I. Dutta, M. H. Reno and I. Sarcevic, 2000]
interesting applicationsastrophysical diagnostics: characterize sources[L. A. Anchordoqui, H. Goldberg, F. Halzen and T. J. Weiler, 2005, T. Kashti and E. Waxman, 2005]
learn about ν properties [H. Athar, M. Jezabek and O. Yasuda, 2000, P. Bhattacharjee and N. Gupta, 2005,
P. D. Serpico and M. Kachelrieß, 2005, J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, 2002, W. Winter, 2006]
Examplepion decay → (1,2,0)neutron beam source → (1,0,0) [L. A. Anchordoqui et al., 2003, P. D. Serpico and M. Kachelrieß, 2005]
muon-damped νµ sources from π decay → (0,1,0)[J. P. Rachen and P. Meszaros, 1998, T. Kashti and E. Waxman, 2005]
optically thick sources → (φνe , φνµ, φντ
) ?
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 23 / 34
Spectra from a single source Flavor content
Flavor Content at the source
Flavor ratio: R0 = φνµ/(φνe + φντ )
depends on the reaction → optically thin source: R0 = Rπ ≈ 2
optically thick sources: strong energy dependencex < xπ
cr → R0 = Rπ ≈ 2xπ
cr <∼ x <∼ xKcr → R0 = RK > 2⇒ bump
xKcr < x → R0 = Rch ≈ 1
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 24 / 34
Spectra from a single source Flavor content
Flavor Content at the source
Flavor ratio: R0 = φνµ/(φνe + φντ )
depends on the reaction → optically thin source: R0 = Rπ ≈ 2optically thick sources: strong energy dependence
x < xπcr → R0 = Rπ ≈ 2
xπcr <∼ x <∼ xK
cr → R0 = RK > 2⇒ bumpxK
cr < x → R0 = Rch ≈ 1
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 24 / 34
Spectra from a single source Flavor content
Flavor Content at the source
Flavor ratio: R0 = φνµ/(φνe + φντ )
depends on the reaction → optically thin source: R0 = Rπ ≈ 2optically thick sources: strong energy dependence
x < xπcr → R0 = Rπ ≈ 2
xπcr <∼ x <∼ xK
cr → R0 = RK > 2xK
cr < x → R0 = Rch ≈ 1
⇓bump at x ≈ xK
cr
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 25 / 34
Spectra from a single source Flavor content
Flavor Content at the Earth
Flavor ratio: R0 + ν oscillation → R = φDνµ
/(φDνe
+ φDντ
)
φDνα
=∑
β Pαβφνβ⇒ R depends on the ν mixing parameters (θij , δCP)
mainly on θ23
⇓
presence of a bump → information on
source: cross-over π − K decayν’s: sensitivity to the θ23 octant
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 26 / 34
Spectra from a single source Flavor content
Flavor Content at the Earth
Flavor ratio: R0 + ν oscillation → R = φDνµ
/(φDνe
+ φDντ
)
φDνα
=∑
β Pαβφνβ⇒ R depends on the ν mixing parameters (θij , δCP)
mainly on θ23
⇓
presence of a bump → information on
source: cross-over π − K decayν’s: sensitivity to the θ23 octant
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 26 / 34
Summary
Summary
High Energy Neutrinospenetrating power + no deflection → ideal astronomical messengers:UHECRs sources, ...
complementary source of ν’s → neutrino properties: mixing, CP, ...
↓
Optically Thick SourcesNeutrino yield
multiple scattering⇒WB limit avoidedif density is too high⇒ HEν’s from π and K decay suppressed
Flavor ratio depends strongly on the energybump shows up at the cross-over between π and K
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 27 / 34
Presence of magnetic fields (work in progress ...)
Presence of magnetic fields (work in progress ...)
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 28 / 34
Presence of magnetic fields (work in progress ...)
Presence of magnetic fields (work in progress ...)
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 29 / 34
Neutrino Spectra
Neutrino Spectra
Assumptions:
injected proton spectrum:
dNp/dE ∝ E−α
α = 2 , E < 10−18 eVα = 2.7 , E > 10−18 eV
[V. Berezinsky, A. Gazizov and S. Grigorieva, 2004]
source: homogeneous slab filled with thermal photons
characterized by
T = 104 K, . . . , 107 KL = 1010 cm, . . . , , 1016 cm
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 30 / 34
Diffuse neutrino spectra from uniform sources
Diffuse neutrino spectra from uniform sources
Fν(E) = 14π
∫∞0
dzH(z)
Lν(z, Eg)
Lν(z, Eg): number of ν’s emitted per comoving volume, time and energywith generation energy Eg = E(1 + z)
Lν(z, Eg) = η(z)Jν(Eg)
Jν(Eg): neutrino spectra from a single sourceη(z): number of sources per co-moving volume and per unit of time
H(z): Hubble parameter, H(z)2 = H20 [Ωm(1 + z)3 + ΩΛ]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 31 / 34
Diffuse neutrino spectra from uniform sources
Constraints
UHECR spectrum (AGASA) ⇒ limits on the proton spectra emitted⇒ Jν(E)→ optically thin sources
(AMANDAII) → sources with τ & 1
EGRET observations ⇒ limits on the electromagnetic cascade produced:
ωcas = femEtot∫∞
0dz
H(z)η(z) ≤ ωobs = 2× 10−6 eV/cm3
[R. Aloisio, V. Berezinsky and M. Kachelrieß, 2004]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 32 / 34
Diffuse neutrino spectra from uniform sources
Constraints
UHECR spectrum (AGASA) ⇒ limits on the proton spectra emitted⇒ Jν(E)→ optically thin sources
current limits on ν fluxes (AMANDAII) → sources with τ & 1
EGRET observations ⇒ limits on the electromagnetic cascade produced:
ωcas = femEtot∫∞
0dz
H(z)η(z) ≤ ωobs = 2× 10−6 eV/cm3
[R. Aloisio, V. Berezinsky and M. Kachelrieß, 2004]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 32 / 34
Diffuse neutrino spectra from uniform sources
Constraints
UHECR spectrum (AGASA) ⇒ limits on the proton spectra emitted⇒ Jν(E)→ optically thin sources
current limits on ν fluxes (AMANDAII) → sources with τ & 1
EGRET observations ⇒ limits on the electromagnetic cascade produced:
ωcas = femEtot∫∞
0dz
H(z)η(z) ≤ ωobs = 2× 10−6 eV/cm3
[R. Aloisio, V. Berezinsky and M. Kachelrieß, 2004]
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 32 / 34
Diffuse neutrino spectra from uniform sources
Constraints
T = 105 k and τ << 1
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 33 / 34
Diffuse neutrino spectra from uniform sources
Constraints
T = 105 k and τ & 1
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 34 / 34
Diffuse neutrino spectra from uniform sources
Constraints
T = 107 k and τ 1
R. Tomàs (AHEP Group -IFIC) High energy neutrinos from astrophysical sources JIGSAW 2007 35 / 34
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