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The domain of radiatively driven mass loss in the H-R diagram

Published online by Cambridge University Press:  14 August 2015

David C. Abbott
David C. Abbott*
Affiliation:
Washburn Observatory University of Wisconsin - Madison Madison, WI 53706

Extract

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Previous work by Castor, Abbott, and Klein (1975) presented a self-consistent model of a steady-state stellar wind. They also showed qualitatively that for O stars at least a static atmosphere could not exist. This paper extends that result by calculating in detail the minimum luminosity as a function of effective temperature required for the line radiation force to exceed gravity. Within the observational and theoretical uncertainty there is a one-to-one correspondence between a star's calculated ability to self-initiate a stellar wind by radiation pressure alone and the observed presence of outflowing material in the UV resonance lines.

Type
Session 5: Theory and Mass Loss Rates Binary Stars - Miscellaneous Topics
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 235 - 240
Copyright
Copyright © Reidel 1979 

References

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