Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-12-01T09:06:32.398Z Has data issue: false hasContentIssue false
  • English
  • Français

Hydrodynamical Models of Rotating Magnetic Winds

Published online by Cambridge University Press:  14 August 2015

Paul K. Barker
Paul K. Barker*
Affiliation:
The University of Western Ontario

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Numerical investigations of rotating stellar winds driven by a combination of magnetic and line radiation forces show a clear dichotomy: shallow winds have their azimuthal velocity enhanced by magnetic corotation, whereas steep winds may have a diminished circular velocity.

Type
VIII. Atmospheric Models
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 485 - 488
Copyright
Copyright © Reidel 1982 

References

Abbott, D.C. 1977, , University of Colorado.Google Scholar
Barker, P.K. 1979, , University of Colorado.Google Scholar
Castor, J.I., Abbott, D.C., and Klein, R.I. 1975, Astrophys. J., 195, p. 157.CrossRefGoogle Scholar
Limber, D.N. 1974, Astrophys. J., 192, p. 429.Google Scholar
Saito, M. 1974, Publ. Astron. Soc. Japan, 26, p. 103.Google Scholar
Weber, E.J., and Davis, L. 1967, Astrophys. J., 148, p. 217.Google Scholar