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Astrophysics and Space Science

, Volume 224, Issue 1–2, pp 541–542 | Cite as

The geometry of decoupled line driven winds

  • John M. Porter
  • Janet E. Drew
Poster Contributions
  • 20 Downloads

Abstract

Bjorkman & Cassinelli (1993) have proposed a mechanism that is expected to produce strong equatorial focusing of the radiation-driven winds from rapidly-rotating B stars. Here the possibility of the decoupling of the stellar radiation field and the outflow is considered. We find that greater equator to pole density ratios may be generated than the standard model, bringing it more into line with results implied by observations.

Key words

Be stars wind mass loss 

References

  1. Bjorkman, J. E., Cassinelli, J.P., 1993, Astrophysical Journal, 409, 429Google Scholar
  2. Castor, J. I., 1987, inInstabilities in Luminous Early-Type Stars, eds. H. J. G. L. M. Lamers & C. W. H. de Loore, D. Reidel, The Netherlands, p159Google Scholar
  3. Owocki, S.P., Castor, J.I., Rybicki G.B., 1988, Astrophysical Journal, 335, 914Google Scholar
  4. Porter, J. M., Drew, J. E., 1994,A&A, in pressGoogle Scholar
  5. Springmann, U. W. E., Pauldrach, A. W. A., 1992,A&A, 262, 515Google Scholar

Copyright information

© Kluwer Academic Publishers 1995

Authors and Affiliations

  • John M. Porter
    • 1
  • Janet E. Drew
    • 1
  1. 1.Astrophysics, Nuclear and Astrophysics laboratoryOxfordU.K.

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