Structure and variability of hot-star winds

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A study of the structure of hot stars and the nature of their variability is presented. We propose a three-phase model for hot-star winds and calculate the X-ray line emission of the hot component of the wind in comparison with the XMM Newton X-ray spectrum of O4f star  Puppis. The results of high-resolution spectroscopy for some bright O stars are also presented. The line profile variability of bright O stars 19 Cep and  Ori A is detected.

Keywords: Spectra of O-B stars; X-ray hot plasma

Document Type: Research Article


Affiliations: 1: Department of Astronomy University of Wisconsin 475 N. Charter Street Madison Wisconsin 53711 USA 2: Nizhnyi Arkhyz Special Astrophysical Observatory Karachaevo-Cherkessiy 369169 Russia 3: St Petersburg University Astronomical Institute St Petersburg Universiteskij Prospect 28 198504 Russia 4: University of Glasgow Department of Physics and Astronomy Glasgow G12 8QQ UK

Publication date: August 1, 2003

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