We derive light curves for the hard gamma-ray emission, at energies up to
several TeV, expected from the unique pulsar/Be-star binary system PSR
B1259-63. This is the only known system in our galaxy in which a radio pulsar
is orbiting a main sequence star. We show that inverse Compton emission from
the electrons and positrons in the shocked pulsar wind, scattering target
photons from the Be star, produces a flux of hard gamma-rays that should be
above the sensitivity threshold of present day atmospheric Cerenkov detectors.
Furthermore, we predict that the flux of hard gamma-rays produced via this
mechanism has a characteristic variation with orbital phase that should be
observable, and which is not expected from any other mechanism.Comment: To be published in Astroparticle Physics. 24 pages, 8 figure