Inverse Compton emission of TeV gamma rays from PSR B1259-63

We derive light curves for the hard gamma-ray emission, at energies up to s everal TeV, expected from the unique pulsar/Bestar 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 t he electrons and positrons in the shocked pulsar wind, scattering target ph otons from the Be star, produces a flux of hard gamma-rays that should be a bove the sensitivity threshold of present day atmospheric Cerenkov detector s. Furthermore, we predict that the flux of hard gamma-rays produced via th is mechanism has a characteristic variation with orbital phase that should be observable, and which is not expected from any other mechanism, (C) 1999 Elsevier Science B.V.