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Mass Loss Phenomena: Hot Stars – Recent Observations and Theoretical Implications

Published online by Cambridge University Press:  30 March 2016

L.B. Lucy
L.B. Lucy*
Affiliation:
Department of Astronomy, Columbia University, New York, NY 10027, USA

Extract

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In the last decade or so, significant progress has been made in developing the theory of the winds of early-type stars. This theory, as is by now well known, is built on the basic assumption that selective radiation pressure, acting in general through a multitude of lines, is responsible both for the expulsion of matter from these stars' atmospheres and for its subsequent acceleration to beyond escape velocity (Lucy and Solomon 1970; Castor, Abbott and Klein 1975; Weber 1981). In order to investigate the effects presumed to be dominant as well as to keep within reasonable bounds the effort required to compute complete models and work out their observational implications, contributors to this line of research have concentrated on a simplified version of the general problem. Thus, for the gas dynamic part of the problem, spherically symmetric flow has usually been assumed and time-dependent effects neglected while, for the radiative transfer part, the Sobolev approximation has usually been adopted and multiple scattering effects neglected. The validity of these assumptions and approximations, and indeed of the whole enterprise, is of course ultimately a matter of observational test.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 6: Highlights of Astronomy. As presented at the XVIIIth General Assembly of the IAU, 1982 , 1983 , pp. 541 - 548
Copyright
Copyright © Reidel 1983

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