High-energy spectra of bursting neutron stars

Details High-energy spectra of bursting neutron stars High-energy spectra of bursting neutron stars

Dec 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299..479y&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 479-486. Research supported by the Minerva Foundation

Astronomy and Astrophysics

Astrophysics

1

Atmospheric Models, Energy Spectra, Neutron Stars, Stellar Atmospheres, Stellar Spectra, X Ray Sources, Annihilation Reactions, Compton Effect, Electron-Positron Pairs, Gamma Rays, High Temperature, Hydrogen Plasma

Scientific paper

Two classes of model atmospheres of bursting neutron stars are considered. (1) atmospheres heated to temperatures of a few keV which can be related to X-ray bursters, and (2) atmospheres heated to relativistic temperatures which are thus more related to gamma-ray bursters. The spectral evolution of the photon flux is calculated, taking into account the most important radiation mechanisms. It is shown that in the low-temperature class of models, backwarming effects play an important role in the formation of the emergent spectrum. Comptonization tends to 'harden' the spectrum even more, although this effect is less significant. In the models with mildly relativistic temperatures, electron-positron pairs may produce an observable 'signature' in the emergent spectrum. The conditions under which either the pair density increases during the burst to some maximum value and then decreases again, or a runaway develops, with the density of pairs increasing exponentially are determined.

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