Inverse Compton Emission of TeV Gamma Rays from PSR B1259-63

Details Inverse Compton Emission of TeV Gamma Rays from PSR B1259-63 Inverse Compton Emission of TeV Gamma Rays from PSR B1259-63

1998-08-12

arxiv.org/abs/astro-ph/9808112v1

Astropart.Phys.10:31-45,1999

Astronomy and Astrophysics

Astrophysics

To be published in Astroparticle Physics. 24 pages, 8 figures

Scientific paper

10.1016/S0927-6505(98)00041-3

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.

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