Magnetic Compton scattering near a hot neutron star polar cap

Abstract

We present results of a model for the energetics of electrons accelerated away from a neutron star polar cap by the large electric fields generated by the rotating highly magnetized neutron star. The energy loss mechanisms we consider in our calculations include magnetic Compton scattering of thermal x-ray photons, triplet pair production, and curvature radiation emission. The electron acceleration mechanism is assumed to operate only to a height above the polar cap approximately equal to the polar cap radius. We find several interesting results. First, magnetic Compton scattering is the dominant energy loss process when the electron Lorentz factors are below 10 7 for typical gamma-ray pulsar magnetic fields and surface temperatures. The amount of energy converted to photons by accelerated electrons ranges from ∼ 10–100% of γ 0mc 2 for pulsar parameters similar to those observed where γ 0 is the maximum Lorentz factor an electron can attain with no radiative losses. We also find that if B>10 13 G and T>3×10 6 K, the Lorentz factors of the electrons can be limited to values of 10 2 – 10 3 assuming values for the size of the neutron star thermal polar cap comparable to the polar cap size determined by the open field lines. Such small Lorentz factors may be capable of explaining the gamma-ray emission from PSR 1509-58 which is observed only to about 1 MeV.