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ABSTRACT  At least one massive binary system containing an energetic pulsar, PSR B1259−63/SS2883, has been recently detected in the TeV γ‐rays by the HESS telescopes. These γ‐rays are likely produced by particles accelerated in the vicinity of the pulsar and/or at the pulsar wind shock, in comptonization of soft radiation from the massive star. However, the process of γ‐ray production in such systems can be quite complicated due to the anisotropy of the radiation field, complex structure of the pulsar wind termination shock and possible absorption of produced γ‐rays which might initiate leptonic cascades. In this paper, we consider in detail all these effects. We calculate the γ‐ray light curves and spectra for different geometries of the binary system PSR B1259−63/SS2883 and compare them with the TeV γ‐ray observations. We conclude that the leptonic inverse‐Compton model, which takes into account the complex structure of the pulsar wind shock due to the aspherical wind of the massive star, can explain the details of the observed γ‐ray light curve.

γ‐rays from binary system with energetic pulsar and Be star with aspherical wind: PSR B1259−63/SS2883