  In gamma-ray binaries neutron star is orbiting a companion that produces a
strong stellar wind. We demonstrate that observed properties of "stellar
wind"-"pulsar wind" interaction depend both on the overall wind thrust ratio,
as well as more subtle geometrical factors: the relative direction of the
pulsar's spin, the plane of the orbit, the direction of motion, and the
instantaneous line of sight. Using fully 3D relativistic magnetohydrodynamical
simulations we find that the resulting intrinsic morphologies can be
significantly orbital phase-dependent: a given system may change from
tailward-open to tailward-closed shapes. As a result, the region of unshocked
pulsar wind can change by an order of magnitude over a quarter of the orbit. We
calculate radiation maps and synthetic light curves for synchrotron (X-ray) and
Inverse-Compton emission (GeV-TeV), taking into account $\gamma-\gamma$
absorption. Our modeled light curves are in agreement with the phase-dependent
observed light curves of LS5039.
