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Gamma-ray binaries are systems that emit non-thermal radiation peaking atenergies above 1 MeV. One proposed scenario to explain their emission consistsof a pulsar orbiting a massive star, with particle acceleration taking place inshocks produced by the interaction of the stellar and pulsar winds. We developa semi-analytical model of the non-thermal emission of the colliding-windstructure including the dynamical effects of orbital motion. We apply the modelto a general case and to LS 5039. The model consists of a one-dimensionalemitter the geometry of which is affected by Coriolis forces owing to orbitalmotion. Two particle accelerators are considered: one at the two-wind standofflocation, and the other one at the turnover produced by the Coriolis force.Synchrotron and inverse Compton emission is studied, accounting for Dopplerboosting and absorption processes associated to the massive star. If bothaccelerators are provided with the same energy budget, most of the radiationcomes from the region of the Coriolis turnover and beyond, up to a few orbitalseparations from the binary system. The model allows us to reproduce some ofthe LS 5039 emission features, but not all of them. In particular, the MeVradiation is probably too high to be explained by our model alone, the GeV fluxis recovered but not its modulation, and the radio emission beyond the Coriolisturnover is too low. The predicted system inclination is consistent with thepresence of a pulsar in the binary. The model is quite successful inreproducing the overall non-thermal behavior of LS 5039. Some improvements aresuggested to better explain the phenomenology observed in this source, likeaccounting for particle reacceleration beyond the Coriolis turnover, unshockedpulsar wind emission, and the three-dimensional extension of the emitter.

A dynamical and radiation semi-analytical model of pulsar-star colliding winds along the orbit: Application to LS 5039