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Stellar winds of hot stars

Published online by Cambridge University Press:  10 September 2015

Ph. Stee  and
O. Chesneau
Ph. Stee
Affiliation:
Observatoire de la Côte d*Azur, CNRS, Boulevard de l*Observatoire, CS 34229, 06304 Nice Cedex 4, France
O. Chesneau*
Affiliation:
Observatoire de la Côte d*Azur, CNRS, Boulevard de l*Observatoire, CS 34229, 06304 Nice Cedex 4, France
*
†O. Chesneau passed away before seeing this article he was involved in.
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Abstract

In this paper, we summarize the basic properties of radiative stellar winds from the theoretical and observational point of views. We illustrate two examples of a radiative code applied to stellar physics: the SIMECA code successfully used to constrain the physics of the circumstellar environment of the Be star α Arae constrained by VLTI-AMBER spectrally resolved measurements and the CMFGEN code applied to the BA supergiants Deneb and Rigel constrained by CHARA-VEGA measurements.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 70: What the Highest Angular Resolution Can Bring to Stellar Astrophysics? , 2014 , pp. 197 - 207
Copyright
© EAS, EDP Sciences, 2015

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