出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Gamma-ray binaries emit GeV and TeV gamma-ray radiation modulated with their orbital period. They may be formed of a young, non accreting pulsar orbiting a massive luminous star. The gamma-ray emission results from the Compton upscattering of stellar photons on relativistic electron-positron pairs efficiently accelerated, possibly where the stellar wind collides with the pulsar wind. Yet, the precise modeling of the spectral and temporal 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 discuss the GeV gamma-ray emission detected in the microquasar Cygnus X-3 and its possible origin.
