Generation of periodical gamma radiation in binary system with a millisecond pulsar

Details Generation of periodical gamma radiation in binary system with a millisecond pulsar Generation of periodical gamma radiation in binary system with a millisecond pulsar

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410..822c&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 822-826 (1997).

Computer Science

1

Pulsars, X-Ray Binaries, Gamma-Ray Sources, Gamma-Ray Bursts

Scientific paper

Consider binary system with a millisecond pulsar ejecting relativistic particles and an optical star emitting soft photons with the energy ω~=1-10 eV. These low energy photons are scattered by the relativistic electrons and positrons of the pulsar's wind. The scattered photons forms a wide spectrum from X-ray band up to ɛ~=1-1000 GeV. The luminosity of gamma radiation Lγ=Lγ(ψ) depends heavily on the angle ψ between the directions to the optical star and to the observer from the pulsar, even when the pulsar wind is isotropic. During the orbital motion this angle varies periodically giving rise to the periodical change of the observed intensity of the gamma radiation and its spectrum. We have calculated the spectral shape Lγ(ɛ,ψ) of the scattered hard photons. Under the assumption that the energy losses of the relativistic particles are small we receive analytical formulas. We apply our results to the binary system PSR B1259-63 and show that if the wind from the Be star is accounted for then it is possible to reproduce the observed spectrum.

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