Relativistic fluid modelling of gamma-ray binaries

Context. We have presented a numerical model for the non-thermal emission of gamma-ray binaries in pulsar-wind driven scenario. Aims. apply this to one best-observed binaries, LS 5039 system. Methods. The involves joint simulation pulsar- and stellar-wind interaction transport electronic pairs from pulsar wind accelerated at emerging shock structure. compute synchrotron inverse Compton post-processing step, while consistently accounting relativistic beaming $\gamma \gamma$-absorption stellar radiation field. Results. stellar- leads formation an extended, asymmetric collision region developing strong shocks, turbulent mixing, secondary shocks flow. Both structure resulting particle distributions show significant orbital variation. Next acceleration particles bow-like Coriolis naturally accounts reacceleration contributing very-high-energy (VHE) gamma-rays. successfully reproduces main spectral features 5039. While predicted lightcurves high-energy VHE band are good agreement with observations, our still does not reproduce X-ray low-energy modulation, which we attribute employed magnetic field model. Conclusions. observed multiband, thus further substantiates wind-driven interpretation binaries. Open issues relate might be addressed through magnetohydrodynamic extension