Modelling of X-ray emission from WR + O binary systems

Details Modelling of X-ray emission from WR + O binary systems Modelling of X-ray emission from WR + O binary systems

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.260..221m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 260, no. 1, p. 221-240.

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37

Astronomical Models, Binary Stars, Emission Spectra, O Stars, Wolf-Rayet Stars, X Ray Binaries, Compton Effect, Computational Astrophysics, Stellar Composition, Stellar Winds, X Ray Absorption

Scientific paper

The structure and X-ray characteristics of the interaction region of colliding stellar winds are analyzed for the case of a WR + O binary system, with allowance made for the effect of stellar wind acceleration and energy losses by radiation and Comptonization as well as the different chemical compositions of stars. It is shown that energy losses by free-free emission underestimate the total energy losses due to thermal emission. It is also shown that the stellar wind acceleration effects can substantially change the gas dynamical parameters in the interaction region and, therefore, the X-ray emission. These effects are very important for close WR + O binary systems, in which the contribution of the shocked O-star wind gas to the total X-ray emission may be dominant.

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