  (abridged) Gamma-ray binaries are massive stars with compact object
companions that are observed to emit most of their energy in the gamma-ray
range. One of these binaries is known to contain a radio pulsar, PSR B1259-63.
Synchrotron and inverse Compton emission from particles accelerated beyond the
light cylinder in striped pulsar winds has been proposed to explain the X-ray
to high energy (HE, $>$ 100 MeV) gamma-ray emission from isolated pulsars. This
pulsar model extends naturally to binary environments, where seed photons for
inverse Compton scattering are provided by the companion star. Here, we
investigate the possibility of gamma-ray emission from PSR B1259-63 in the
framework of the striped pulsar wind model. The orbital geometry of PSR
B1259-63 is well constrained by observations and the double radio pulse
suggests an almost orthogonal rotator so that the solid angle covered by the
striped region is close to $4\pi$. We calculate the orbital and rotational
phase-resolved spectral variability and light-curves to expect.
