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Massive stars at (very) high energies: γ-ray binaries

Published online by Cambridge University Press:  12 July 2011

Guillaume Dubus  and
Benoît Cerutti
Guillaume Dubus
Affiliation:
Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université J. Fourier & CNRS, France email: gdubus@obs.ujf-grenoble.fr
Benoît Cerutti
Affiliation:
Laboratoire d'Astrophysique de Grenoble, UMR 5571 Université J. Fourier & CNRS, France email: gdubus@obs.ujf-grenoble.fr
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Abstract

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γ-ray binaries are systems that emit most of their radiative power above 1 MeV. They are associated with O or Be stars in orbit with a compact object, possibly a young pulsar. Much like colliding wind binaries, the pulsar generates a relativistic wind that interacts with the stellar wind. The result is non-thermal emission from radio to very high energy γ-rays. The wind, radiation and magnetic field of the massive star play a major role in the dynamics and radiative output of the system. They are particularly important to understand the high energy physics at work. Inversely, γ-ray binaries offer novel probes of stellar winds and insights into the fate of O/B binaries.

Keywords

radiation mechanisms: nonthermalpulsars: generalstars: windsoutflowsgamma rays: observationsgamma rays: theoryX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 581 - 586
Copyright
Copyright © International Astronomical Union 2011

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