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Can Hot Star Winds be Driven by Radiation Pressure?

  • Marc Leroy
  • Jean-Pierre J. Lafon
Part of the Astrophysics and Space Science Library book series (ASSL, volume 89)

Abstract

The mechanisms by which early type (O and B) stars loose mass is investigated. The phenomena occuring close to the photosphere are crucial for the structure of the wind. It is shown that the effects of radiation are not sufficient to explain the observed winds. A general scheme for energy balance including a corona is proposed.

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References

  1. Cassinelli, J.P., OlsonG.: 1979, Astrophys. J. 229, 304.ADSCrossRefGoogle Scholar
  2. Castor, J.I., Abbott, D.C., Klein, R.I.: 1975, Astrophys. J. 195, 157.ADSCrossRefGoogle Scholar
  3. Leroy, M., Lafon J.P.J. — Can hot star winds be driven by radiation pressure? I and II. — On the importance of boundary conditions and non local properties of radiative transfer coupled with hydrodynamics in hot star winds. Rpt DESPA 202 Observatoire de Meudon; 92190 Meudon (France)Google Scholar
  4. Mihalas, D., Kunasz, P.B., Hummer, D.G.: 1976, Astrophys. J. 210, 419.ADSCrossRefGoogle Scholar

Copyright information

© D. Reidel Publishing Company 1981

Authors and Affiliations

  • Marc Leroy
    • 1
  • Jean-Pierre J. Lafon
    • 1
  1. 1.Départment Recherches SpatialesObservatoire de Meudon; Laboratoire Associé du CNRS n° 264MeudonFrance

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