Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2011-07-22
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
Changes in Title name, Fig.2, Fig.3. More references added
Scientific paper
In the internal shock model of gamma ray bursts ultrahigh energy pions, muons, kaons and neutrons are likely to be produced in the interactions of shock accelerated relativistic protons with low energy photons (KeV-MeV). These particles subsequently decay to high energy neutrinos/antineutrinos and other secondaries. In the high internal magnetic fields of gamma ray bursts, the ultrahigh energy charged particles ($\pi^+$, $\mu^+$, $K^+$) lose energy significantly due to synchrotron radiations before decaying into secondary high energy neutrinos and antineutrinos. The charged kaons being heavier than pions, lose energy slowly and their secondary neutrino flux is more than that from pions and muons at very high energy. The relativistic neutrons decay to high energy antineutrinos, protons and electrons.We have calculated the total neutrino flux (neutrino and antineutrino) considering the decay channels of ultrahigh energy pions, muons, kaons and neutrons. We show that depending on the values of the parameters of a gamma ray burst the antineutrino flux generated in neutron decay can exceed the total neutrino flux produced in $\pi^+$ and $\mu^+$ decay. The neutron decay channel may become more important than the $\pi^+$ and $\mu^+$ decay channels of neutrino and antineutrino production at TeV energy.We also discuss that the pion, muon, kaon, and neutron decay channels may show distinct peaks in the total neutrino spectrum at high energies depending on the values of the parameters (luminosity, Lorentz factor, variability time, spectral indices and break energy in the photon spectrum) of a gamma ray burst.
Gupta Nayantara
Moharana Reetanjali
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