Other
Scientific paper
Jun 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..388..213o&link_type=abstract
Mass Loss from Stars and the Evolution of Stellar Clusters ASP Conference Series, Vol. 388, proceedings of the conference held 2
Other
Scientific paper
The X-ray spectra of O stars show characteristic emission-line profiles. Their shape results from the attenuation of the X-ray emission by the inhomogenous wind material, and can be reproduced by adequate models. The wind absorption in Wolf-Rayet type stars is at least an order of magnitude higher than in O-type stars. This high wind absorption was suggested to explain the lack of X-ray emission from WC-type stars. Winds of WN stars are less opaque for X-ray than winds of WC stars. Some putatively single WN stars are detected in X-rays, while others are not. It is presently unclear whether wind absorption alone can account for the different levels of X-ray emission observed in WR stars. -- The profile of the N VII resonance line in the X-ray spectrum of ζ Puppis shows a self-absorption feature, indicating that the hot X-ray emitting plasma is optically thick.
Feldmeier Achim
Hamann Wolf-Rainer
Oskinova Lida M.
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