High Energy Neutrinos from Astrophysical Sources Dmitry Semikoz UCLA, Los Angeles & INR, Moscow.
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Transcript of High Energy Neutrinos from Astrophysical Sources Dmitry Semikoz UCLA, Los Angeles & INR, Moscow.
High Energy Neutrinos High Energy Neutrinos from Astrophysical from Astrophysical
Sources Sources
Dmitry SemikozDmitry SemikozUCLA, Los Angeles & INR, MoscowUCLA, Los Angeles & INR, Moscow
Ultra High Energy \\ Cosmic Rays
Neutrino Oscillation Workshop, September 16, 2004
Overview: Introduction: cosmic rays, gamma-rays and neutrinos Diffuse neutrino fluxes
Neutrinos from UHECR (Friday, F.Halzen , G.Miele) Neutrinos from AGN
Most probable point-like neutrino sources AGN Galaxy center Microquasars SuperNova high energy E>TeV neutrinos GRB (Friday, P.Meszaros)
Conclusion
Neutrino Oscillation Workshop, September 16, 2004
INTRODUCTION
Neutrino Oscillation Workshop, September 16, 2004
Conditions required for production of high energy neutrinos in astrophysical sources:
Acceleration of charged particles (protons or nuclei) to high energies E>1015 eV
Accelerated particles should lose energy through pion production or neutron decay
Obey gamma-ray and neutrino flux limits
1 pBBnR
Neutrino Oscillation Workshop, September 16, 2004
Neutrinos from pion production
ee
...
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i
b
i
b
PP
NN
p
n
20
eepn
Conclusion: photon and neutrino fluxes are connected in well-defined way. If we know one of them we can predict other: tottot EE ~
Neutrino Oscillation Workshop, September 16, 2004
High energy photons from pion decay cascade down in GeV region
Neutrino Oscillation Workshop, September 16, 2004
The high energy gamma ray detector on the Compton Gamma Ray Observatory (20 MeV - ~20 GeV)
EGRET: gamma-ray flux
Neutrino Oscillation Workshop, September 16, 2004
Photon flux at E>100 MeV as measured by EGRET till 1995
The Flux of Diffuse Photons Point sources
Neutrino Oscillation Workshop, September 16, 2004
The next-generation ground-based and space-based experiments are well matched.
Complementary capabilities
ground-based space-based ACT EAS Pairangular resolution good fair goodduty cycle low high higharea large large smallfield of view small large large+can reorient
energy resolution good fair good, w/ smaller systematic uncertainties
High energy gamma ray experiments
Neutrino Oscillation Workshop, September 16, 2004
EGRET flux can consist of:
Inverse Compton scattered photons Synchrotron photons from high energy
protons Photons from pion decay, which cascade
down in intergalactic space or in source Thus EGRET flux give just upper limit on
diffuse or point source neutrino flux
Neutrino Oscillation Workshop, September 16, 2004
Diffuse flux of neutrinos
Neutrino Oscillation Workshop, September 16, 2004
Cosmic rays and AGNs
Diffused flux from cosmic rays Many unresolved sources
AMANDA II
Neutrino Oscillation Workshop, September 16, 2004
GLAST: 10000 sourcesLAT 1st Catalog: >9000 sources possible
Neutrino Oscillation Workshop, September 16, 2004
AGN as neutrino sources
Neutrino Oscillation Workshop, September 16, 2004
Only few classes of astrophysical objects are able to accelerate particles to highest energies
For neutrino production we have to look for the sources with high density of background photons or protons
Neutrino Oscillation Workshop, September 16, 2004
Can sources accelerate protons to such high energies? AGASA data E> 1019 eV:
AGNs are one of most probable sources
Neutrino Oscillation Workshop, September 16, 2004
Neutrino production in AGN core
Neutrino Oscillation Workshop, September 16, 2004
Neutrinos from AGN core
AMANDA II
J.Alvarez-Muniz and P.Mezsaros, astro-ph/0409034
Neutrino Oscillation Workshop, September 16, 2004
Most probable point-like neutrino
sources
Neutrino Oscillation Workshop, September 16, 2004
Point source fluxes
Background of atmospheric neutrinos against flux of given source. Position of source given a priori.
AMANDA II 1.8 degrees resolution: 3 background 6 observed
ANTARES 0.3 degrees ICECUBE 0.5 degrees KM^3 0.3 degrees<
Neutrino Oscillation Workshop, September 16, 2004
Most probable single sources- AGN
Blazars GeV-loud Optical depth for
protons should be large:
pnR
Only 22 sources from 66 are GeV - loud
Neutrino Oscillation Workshop, September 16, 2004
TeV blazars does not obey last condition
Indeed, in order TeV blazars be a neutrino sources:
pnR nRp= 6x10-28cm2 while for TeV gamma-rays
= 6.65 x 10-25cm2
CONTRADICTION!!! Except if proton background density is as high as photon one, because pp= 6x10-26cm2 This is unlikely in BL Lacs, where emission lines are absent.
Neutrino Oscillation Workshop, September 16, 2004
Which sources ?
Blazars (angle – energy correlation) Blazars should be GeV loud Optical depth for protons should be large:
pnR No 100 - kpc scale jet detected (model-dependent)
Neutrino Oscillation Workshop, September 16, 2004
Neutrino production in AGN
Neutrino Oscillation Workshop, September 16, 2004
Bound on blazars which can be a neutrino sources
A.Neronov, D.S., 2002
Neutrino Oscillation Workshop, September 16, 2004
Collimation of neutrino flux in compare to GeV flux
AMANDA II
Neutrino Oscillation Workshop, September 16, 2004
Galaxy center: cosmic rays
AGASA experiment see anisotropy towards the Galactic center.
This signal can be explained by neutrons.
Neutrino Oscillation Workshop, September 16, 2004
Galaxy center
Cosmic ray neutrons decay on the way and produce neutrinos.
L.Archadoqui, H.Holdberg, F.Halzen and T.Weiler, astro-ph/0311002
eepn
Neutrino Oscillation Workshop, September 16, 2004
Microquasars
AGN on star scales. Protons are
accelerated by shock wave up to 1016 eV
In interaction with X-ray photons from accretion disk protons produce 1-100 TeV neutrinos
A.Levinson and E.Waxman, 2001C.Distefano et al, 2002
psEFE
1.0
cm
eV10)(
222
Neutrino Oscillation Workshop, September 16, 2004
Galactic SN When shock came out of star it
start to accelerate protons. Up to 200 events with E>1 TeV
in ICECUBE within few hours (E.Waxman and A.Loeb, astro-ph/0102317)
Extra 1000-10000 events in first year (V.Berezinsky and V.Ptuskin, 1988)
Can help to detect SN location up to 0.1 degree. (R.Tomas, D.S., G.Raffelt, M.Kachelriess and A.Dighe, hep-ph/0307050)
Supernova 1987A Supernova 1987A 23 February 198723 February 1987
Neutrino Oscillation Workshop, September 16, 2004
Conclusions Diffuse neutrino flux can be combination of cosmic ray and
AGN neutrinos. GeV-loud blazars with high optical depth for protons are good
candidates for point-like neutrino sources.
Galaxy center can be good source of neutrinos and flux can be predicted based on AGASA signal.
Galactic microquasars, GRB, galactic SN are sources of neutrinos.
We have a good chance to detect those sources with km2 detectors.