Volume 373, Number 3, July III 2001
|Page(s)||1009 - 1018|
|Section||Stellar structure and evolution|
|Published online||15 July 2001|
Modelling X-ray variability in the structured atmospheres of hot stars
Department of Physics and Astronomy, University of Glasgow, Glasgow, G12 8QQ, Scotland UK
2 Department of Physics and Astronomy, University of Iowa, 203 Van Allen Hall, Iowa City, IA 52242, USA
3 Department of Astronomy, University of Wisconsin, 5534 Sterling Hall, 475 N. Charter St., Madison, WI 53706-1582, USA
Corresponding author: L. M. Oskinova, firstname.lastname@example.org
Accepted: 2 May 2001
We describe X-ray production in the atmospheres of hot, early-type stars in the framework of a "stochastic shock model" . The extended envelope of a star is assumed to possess numerous X-ray emitting "hot" zones that are produced by shocks and embedded in the ambient "cold" medium in dynamical equilibrium. It is shown that the apparent lack of X-ray variability on short (~ hours) timescales do not contradict a shock model for X-ray production. The character of the X-ray variability is found to depend on the frequency with which hot zones are generated, the cool wind opacity to X-rays, and the wind flow parameters, such as mass loss rate and terminal speed.
Key words: stars: abundances / stars: early-type / stars: mass-loss / stars: Wolf-Rayet / X-rays: stars
© ESO, 2001
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