Volume 399, Number 3, March I 2003
|Page(s)||1121 - 1134|
|Section||Stellar structure and evolution|
|Published online||14 February 2003|
Gamma-ray emission from Wolf-Rayet binaries
Instituto Argentino de Radioastronomía, C.C.5, (1894) Villa Elisa, Buenos Aires, Argentina
Corresponding author: P. Benaglia, firstname.lastname@example.org
Accepted: 4 December 2002
In the colliding wind region of early-type binaries, electrons can be accelerated up to relativistic energies displaying power-law spectra, as demonstrated by the detection of non-thermal radio emission from several WR+OB systems. The particle acceleration region, located between the stars, is exposed to strong photon fields in such a way that inverse Compton cooling of the electrons could result in a substantial high-energy non-thermal flux. In particular cases, the ratio of the energy densities of magnetic to photon fields in the colliding wind region will determine whether a given source can produce or not significant gamma-ray emission. We present here a study of the binaries WR 140, WR 146, and WR 147 in the light of recent radio and gamma-ray observations. We show that with reasonable assumptions for the magnetic field strength WR 140 can produce the gamma-ray flux from the EGRET source 3EG J2022+4317. WR 146 and WR 147 are below the detection threshold, but new and forthcoming instruments like INTEGRAL and GLAST might detect non-thermal emission from them.
Key words: stars: early-type / stars: binaries: general / stars: winds, outflows / radio continuum: stars / gamma-rays: observations / gamma-rays: theory
© ESO, 2003
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