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Radiatively-Driven Stellar Winds

Published online by Cambridge University Press:  12 April 2016

L.B. Lucy
L.B. Lucy*
Affiliation:
European Southern Observatory Karl-Schwarzschild-Str. 2 D-8046 Garching bei München, Federal Republic of Germany

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In this review, attention will be focussed exclusively on the winds of hot stars, concentrating for the most part on spectral types 0 and B. For these stars, a clear consensus has emerged that it is the gradient of selective radiation pressure - i.e., line-driving - that explains the high terminal velocities, typically ~ 2000 km s−1, of their winds. Accordingly, few would now doubt that the supersonic zones of these winds present us with rather clean examples of line-driven flow, whose investigation therefore properly belongs under the heading “Radiation Hydrodynamics”. Moreover, in marked contrast with other astronomical environments where line-driven winds may exist, the stellar case is geometrically and parametrically well defined and is thus by far the best natural example from which to learn about such flows.

Type
2. Normal Stars
Information
International Astronomical Union Colloquium , Volume 89: Radiation Hydrodynamics in Stars and Compacts Objects , 1986 , pp. 75 - 87
Copyright
Copyright © Springer-Verlag 1986

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