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Chromospheres, Coronae, and Mass Loss in Stars Hotter than the Sun

Published online by Cambridge University Press:  30 March 2016

Theodore P. Snow Jr.
Theodore P. Snow Jr.*
Affiliation:
Laboratory for Atmospheric and Space Physics and Department of Astro-Geophysics, University of Colorado, Boulder, Colorado 80309

Abstract

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Reviews of the mass-loss characteristics of OB stars have been published recently, and the present review therefore emphasizes the A and F stars and very recent results on O and B stars. For the F stars, chromospheric indicators are present in the form of emission lines, seen in visible and ultraviolet wavelengths. Winds are present in A supergiants, but not in main sequence stars, although at least a few of the latter are X-ray sources, indicating the possible existence of coronae. Most OB supergiants are X-ray sources as well, indicating, along with the presence of super-ionization, that these stars have coronae. On the main sequence, the O stars and some B stars (including Be stars in many cases) have mass loss with highly-ionized species in the wind. The winds in the O and B stars are commonly variable. The mass-loss rates do not show a simple dependence on luminosity, contrary to the predictions for radiatively-driven winds.

Type
Joint Discussion
Information
Highlights of Astronomy , Volume 5: Highlights of Astronomy. As presented at the XVIIth General Assembly of the IAU, 1979 , 1980 , pp. 525 - 531
Copyright
Copyright © Cambridge University Press 1980

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