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Empirical wind models from detail ed UV-line fits: Tau Scorpii

Published online by Cambridge University Press:  12 April 2016

W.-R. Hamann
W.-R. Hamann*
Affiliation:
Institut für Theoretische Physik und Sternwarte, Universität Kiel, F.R.G.

Extract

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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).

Type
Session III - Winds From Early Type Stars: Theory
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 161 - 165
Copyright
Copyright © Reidel 1981

References

Cassinelli, J.P., OLSON, G., STALIO, R.: 1978, Astrophys.J. 220, 573 Google Scholar
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Hamann, W.R.: 1980b, Astron.Astrophys in pressGoogle Scholar
Lamers, H.J.G.L.M., Rogerson, J.B.: 1978, Astron.Astrophys. 66, 417 Google Scholar
Simon, K.P. et al.: 1979, in ‘The First Year of IUE’, NASA-ESA-SRC, London Google Scholar