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Physics of Radiatively Driven Winds by High Angular Resolution Observations (HARO)

Published online by Cambridge University Press:  12 April 2016

Ph. Stee ,
D. Bonneau ,
D. Mourard  and
F. Vakili
Ph. Stee
Affiliation:
Equipe GI2T, Département Fresnel, CNRS-UMR 6528, Observatoire de la Côte d’Azur, 2130 route de l’Observatoire, Caussols, 06460 St Vallier de Thiey, France
D. Bonneau
Affiliation:
Equipe GI2T, Département Fresnel, CNRS-UMR 6528, Observatoire de la Côte d’Azur, 2130 route de l’Observatoire, Caussols, 06460 St Vallier de Thiey, France
D. Mourard
Affiliation:
Equipe GI2T, Département Fresnel, CNRS-UMR 6528, Observatoire de la Côte d’Azur, 2130 route de l’Observatoire, Caussols, 06460 St Vallier de Thiey, France
F. Vakili
Affiliation:
Equipe GI2T, Département Fresnel, CNRS-UMR 6528, Observatoire de la Côte d’Azur, 2130 route de l’Observatoire, Caussols, 06460 St Vallier de Thiey, France

Abstract

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Numerous models have been developed during the last two decades which try to fit a small number of “classical” observables as closely as possible (i.e Hα line profile and continuum energy distribution or polarization data). Nevertheless, little has been done to include High Angular Resolution Observations (HARO) in simulations in spite of the fact that such data can strongly constrain radiative wind models. In the following, we shall review recent results coming from HARO of active B stars and we shall focus on our radiative wind model for active hot stars which integrates these measurements.

Type
Section I Observations of Non-spherical Winds
Information
International Astronomical Union Colloquium , Volume 169: Variable and Non-spherical Stellar Winds in Luminous Hot Stars , 1999 , pp. 115 - 118
Copyright
Copyright © Springer-Verlag 1999

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