The gamma-ray binaries LS 5039, LS I +61 303 and PSR B1259-63

Details The gamma-ray binaries LS 5039, LS I +61 303 and PSR B1259-63 The gamma-ray binaries LS 5039, LS I +61 303 and PSR B1259-63

2006-08-12

arxiv.org/abs/astro-ph/0608262v1

Astronomy and Astrophysics

Astrophysics

10 pages, 3 figures, proceedings Vulcano workshop (22nd - 27th May, 2006), Frontier Objects in Astrophysics and Particle Physi

Scientific paper

Three binaries are now established sources of emission at very high energies (>1e11 eV). They are composed of a massive star and a compact object. The emission can be due to the interaction of the relativistic wind from a young ms pulsar with the stellar wind of the companion, by which rotation-power ends up as non-thermal flux. Variations at VHE energies are explained as due to gamma-gamma absorption and/or changes in shock location along the orbit. Resolved radio emission is due to cooling particles trailing the pulsar.

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