High-Energy Neutrinos Produced by Interactions of Relativistic Protons in Shocked Pulsar Winds

Details High-Energy Neutrinos Produced by Interactions of Relativistic Protons in Shocked Pulsar Winds High-Energy Neutrinos Produced by Interactions of Relativistic Protons in Shocked Pulsar Winds

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf..133n&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astronomy

Scientific paper

We have estimated fluxes of neutrinos and gamma-rays that are generated from decays of charged and neutral pions from a pulsar surrounded by supernova ejecta in our galaxy, including an effect that has not been taken into consideration, that is, interactions between high energy cosmic rays themselves in the nebula flow, assuming that hadronic components are the energetically dominant species in the pulsar wind. Bulk flow is assumed to be randomized by passing through the termination shock and energy distribution functions of protons and electrons behind the termination shock are assumed to obey the relativistic Maxwellians. We have found that fluxes of neutrinos and gamma-rays depend very sensitively on the wind luminosity, which is assumed to be comparable to the spin-down luminosity. In the case where B = 1012G and P = 1ms, neutrinos should be detected by km3 high-energy neutrino detectors such as AMANDA and IceCube. Also, gamma-rays should be detected by Cherenkov telescopes such as CANGAROO and H.E.S.S. as well as by gamma-ray satellites such as GLAST.

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