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XMM-Newton observations of PSR B1259–63 near the 2004 periastron passage

Published online by Cambridge University Press:  12 May 2006

M. Chernyakova ,
A. Lutovinov ,
J. Rodriguez  and
S. Johnston
M. Chernyakova
Affiliation:
INTEGRAL Science Data Centre, Chemin d'Écogia 16, 1290 Versoix, Switzerland email: Masha.Chernyakova@obs.unige.ch Geneva Observatory, 51 ch. des Maillettes, CH-1290 Sauverny, Switzerland
A. Lutovinov
Affiliation:
Space Research Institute, 84/32 Profsoyuznaya Street, Moscow 117997, Russia
J. Rodriguez
Affiliation:
INTEGRAL Science Data Centre, Chemin d'Écogia 16, 1290 Versoix, Switzerland email: Masha.Chernyakova@obs.unige.ch CEA Saclay, DSM/DAPNIA/Service d'Astrophysique (CNRS UMR 7158 AIM), 91191 Gif sur Yvette, France
S. Johnston
Affiliation:
Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 1710, Australia.
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Abstract

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We present here the results of new XMM-Newton observations of the PSR B1259–63 system during the beginning of 2004, as the pulsar approaches the disc of the Be star. We combine these results with earlier X-ray data from BeppoSAX, XMM-Newton, and ASCA. The X-ray light curve looks similar to the radio light curve with a rapid increase in the flux around the time of the disc crossing. This supports a model in which the X-ray emission from the system is due to inverse Compton scattering of the pulsar wind relativistic particles with moderate Lorentz factor $\gamma \sim 10$–100 on the Be star soft photons.

Keywords

pulsars: individual: PSR B1259–63 – X-rays: binaries – X-rays: individual: PSR B1259–63
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S230: Populations of High Energy Sources in Galaxies , August 2005 , pp. 78 - 79
Copyright
2006 International Astronomical Union