Non-pulsed emission from the binary system B1259-63

被引：6

作者：

Chernyakova, M ^{[1
]}

Illarionov, A ^{[1
]}

机构：

[1] PN Lebedev Phys Inst, Ctr Astro Space, Moscow, Russia

来源：

ASTROPHYSICS AND SPACE SCIENCE | 2000年 / 274卷 / 1-2期

关键词：

D O I：

10.1023/A:1026508325315

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

PSR B1259-63 is the only known binary system with a radio pulsar from which the non-pulsed radio and X-ray emission was detected. The companion star in this system is a Be star SS 2883. A rapidly rotating radio pulsar is expected to produce a wind of relativistic particles. Be stars are known to produce highly asymmetric mass loss. Due to the interaction of the pulsar wind and the Be star wind the system of two shocks between the pulsar and the Be star forms. In this paper we show that the observed non-pulsed radio emission from the system is a result of the synchrotron emission of the relativistic particles in the outflow beyond the shock wave and that the non-pulsed X-ray emission is due to the inverse Compton scattering of the Be star photons on this particles.

引用

页码：177 / 188

页数：12

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