Non-pulsed gamma radiation from a binary system with a pulsar

被引:22
作者
Chernyakova, MA [1 ]
Illarionov, AF [1 ]
机构
[1] PN Lebedev Phys Inst, Ctr Astro Space, Moscow 117810, Russia
关键词
binaries : general; pulsars : general; pulsars : individual : PSR B1259; 63; X-rays : stars;
D O I
10.1046/j.1365-8711.1999.02356.x
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We consider a binary system with a millisecond pulsar ejecting relativistic particles and an optical star emitting soft photons with energy omega similar or equal to 1-10 eV. These low-energy photons are scattered by the relativistic electrons and positrons of the pulsar wind. The scattered photons form a wide spectrum from the hard X-ray band up to gamma band epsilon similar or equal to 1-1000 GeV. When the pulsar wind is isotropic, the luminosity of gamma radiation L-gamma = L-gamma(psi) depends strongly on the angle psi,between the directions to the optical star and the observer from the pulsar. During the orbital motion this angle varies periodically, giving rise to a periodic change of the observed intensity of the gamma radiation and its spectrum. We calculate the spectral shape of the scattered hard photons. Under the assumption that the energy losses of the relativistic particles are small, we derive analytic formulae for the spectra of the photons. 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.
引用
收藏
页码:359 / 366
页数:8
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