Non-pulsed emission from the binary system PSR B1259-63

Details Non-pulsed emission from the binary system PSR B1259-63 Non-pulsed emission from the binary system PSR B1259-63

2000-04-04

arxiv.org/abs/astro-ph/0004039v1

Astrophys.Space Sci. 274 (2000) 177-188

Astronomy and Astrophysics

Astrophysics

11 pages, Proceedings of the Conference "Progress in Cosmic Gas Dynamics", Moscow, September 13-17, 1999, to be published in "

Scientific paper

10.1023/A:1026508325315

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.

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