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Gamma-ray binaries emit GeV and TeV gamma-ray radiation mod ulated with their orbital period. They may be formed of a young, non accreting pulsar orbi ting a massive luminous star. The gamma-ray emission results from the Compton upscatteri ng of stellar photons on relativistic electron-positron pairs efficiently accelerated, possibl y where the stellar wind collides with the pulsar wind. Yet, the precise modeling of the spectral and te mporal behavior of these binaries in gamma rays remains challenging. Here, we review our current understanding of the production of high-energy radiation in gamma-ray binaries. We also dis cus the GeV gamma-ray emission detected in the microquasar Cygnus X-3 and its possible orig in.

On the origin of the GeV and TeV emission in gamma-ray binaries (invited talk)