Gamma rays from pulsar wind shock acceleration

Details Gamma rays from pulsar wind shock acceleration Gamma rays from pulsar wind shock acceleration

May 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3071..183h&link_type=abstract

In its The Energetic Gamma-Ray Experiment Telescope (EGRET) Science Symposium p 183-199 (SEE N90-23294 16-90)

Physics

Cygnus Constellation, Gamma Ray Spectra, Gamma Rays, Luminosity, Particle Energy, Pulsars, Shock Waves, Supernova Remnants, Electron-Positron Pairs, Gamma Ray Telescopes, Protons

Scientific paper

A shock forming in the wind of relativistic electron-positron pairs from a pulsar, as a result of confinement by surrounding material, could convert part of the pulsar spin-down luminosity to high energy particles through first order Fermi acceleration. High energy protons could be produced by this mechanism both in supernova remnants and in binary systems containing pulsars. The pion-decay gamma-rays resulting from interaction of accelerated protons with surrounding target material in such sources might be observable above 70 MeV with EGRET (Energetic Gamma-Ray Experimental Telescope) and above 100 GeV with ground-based detectors. Acceleration of protons and expected gamma-ray fluxes from SN1987A, Cyg X-3 type sources and binary pulsars are discussed.

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