Comptonization of thermal photons by relativistic electron beams

Details Comptonization of thermal photons by relativistic electron beams Comptonization of thermal photons by relativistic electron beams

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...336..861d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 336, Jan. 15, 1989, p. 861-874. Research supported by the Research Corp.

Astronomy and Astrophysics

Astrophysics

59

Compton Effect, Neutron Stars, Relativistic Electron Beams, Stellar Radiation, Thermal Radiation, Cyclotron Resonance, Energy Distribution, Gamma Ray Spectra, Monte Carlo Method, Pulsars

Scientific paper

This paper presents a numerical calculation of gamma-ray emission produced by Compton scattering of relativistic electron beams on background thermal radiation, which includes spatial dependence of electron energy losses and cyclotron resonance scattering in a strong magnetic field. In the first version, the scattering is described by the fully relativistic Klein-Nishina cross section, but the magnetic field is neglected. In the second version, the scattering is described by the magnetic resonant cross section in the Thomson limit. It is found that when the magnetic field is not included, electron energy losses are important only at higher neutron star surface temperatures (T about 3,000,000 K). In the presence of a strong magnetic field, (10 to the 12th G), resonant scattering greatly increases electron energy losses, making scattering very efficient even at lower surface temperatures. Resulting photon and electron spectra for both cases ae discussed in relation to models for pulsar X-ray and gamma-ray emission.

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