Abstract
The main-sequence BO star Tau Sco has been studied previously by Lamers and Rogerson (1978). However, their line fit was restricted to the blue wings of the UV resonance lines because the line formation was calculated in Sobolev approximation. We now repeat this investigation by means of the comoving-frame (CMF) method, which we have extended to the treatment of overlapping doublets. From a systematic comparison (Hamann 1980b) we know that the results may deviate considerably from those of the Sobolev method. Our method has been applied previously to the other “prototype” of mass loosing early-type stars, the Of star Zeta Puppis (Hamann 1980a).
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References
Cassinelli, J.P., Olson, G., Stalio, R.: 1978, Astrophys. J. 220, 573
Hamann, W.R .: 1980a, Astron. Astrophys. 84, 342
Hamann, W.R.: 1980b, Astron. Astrophys. in press
Lamers, H.J.G.L.M., Rogerson, J.B.: 1978, Astron. Astrophys. 66, 417
Simon, K.P. et al.: 1979, in “The First Year of IUE”, NASA-ESA-SRC, London
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© 1981 D. Reidel Publishing Company
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Hamann, WR. (1981). Empirical Wind Models from Detailed UV-Line Fits: Tau Scorpii. In: Chiosi, C., Stalio, R. (eds) Effects of Mass Loss on Stellar Evolution. Astrophysics and Space Science Library, vol 89. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8500-1_26
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DOI: https://doi.org/10.1007/978-94-009-8500-1_26
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-009-8502-5
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