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

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

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..272..581d&link_type=abstract

Active OB stars: structure, evolution, mass loss, and critical limits, Proceedings of the International Astronomical Union, IAU

Physics

Radiation Mechanisms: Nonthermal, Pulsars: General, Stars: Winds, Outflows, Gamma Rays: Observations, Gamma Rays: Theory, X-Rays: Binaries

Scientific paper

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.

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