Abstract
Mass-loss rates have been determined for 6 hydrogen-deficient stars by modelling their wind line profiles in the UV from high resolution spectra. Line profiles were calculated with using the SEI method (Sobolev approximation with Exact Integration of the transfer equation: Lamers, Cerruti-Sola and Perinotto 1987). Optimum fits to the observations were obtained using a least squares procedure. Results for single helium stars are in good agreement with previous studies. The stellar wind from the binary star υ Sgr has been modelled succesfully for the first time by adopting an extended two component wind.
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References
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© 1992 Springer-Verlag
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Dudley, R.E., Simon Jeffery, C. (1992). Mass loss from υ Sgr and other helium stars. In: Heber, U., Jeffery, C.S. (eds) The Atmospheres of Early-Type Stars. Lecture Notes in Physics, vol 401. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-55256-1_325
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DOI: https://doi.org/10.1007/3-540-55256-1_325
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