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Gamma-ray production in selected Wolf-Rayet binaries

Published online by Cambridge University Press:  26 May 2016

Paula Benaglia  and
Gustavo E. Romero
Paula Benaglia
Affiliation:
Instituto Argentino de Radioastronomía, C.C. 5, 1894 Villa Elisa, Buenos Aires, Argentina
Gustavo E. Romero
Affiliation:
Instituto Argentino de Radioastronomía, C.C. 5, 1894 Villa Elisa, Buenos Aires, Argentina

Abstract

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In the colliding wind region of early-type binaries, electrons can be accelerated up to relativistic energies, as demonstrated by the detection of non-thermal radio emission from several WR+OB systems. The particle acceleration region is exposed to strong photon fields, and inverse-Compton cooling of the electrons could result in a substantial high-energy non-thermal flux. We present here preliminary results of a study of the binaries WR 140, WR 146, and WR 147 in the light of recent radio and γ-ray observations. We show that under reasonable assumptions WR 140 can produce the γ-ray flux from the GRO-egret source 3EG J 2022+4317. WR 146 and WR 147 are below the detection threshold.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 150 - 151
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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