Hostname: page-component-78c5997874-dh8gc Total loading time: 0 Render date: 2024-11-05T19:30:41.189Z Has data issue: false hasContentIssue false

Models of classical Be stars with gravity darkening

Published online by Cambridge University Press:  12 July 2011

Meghan A. McGill
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: [email protected], [email protected], [email protected]
T. A. Aaron. Sigut
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: [email protected], [email protected], [email protected]
Carol E. Jones
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: [email protected], [email protected], [email protected]
Rights & Permissions [Opens in a new window]

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.

Classical Be stars are rapidly rotating, hot stars that possess an equatorial disk formed from gas released by the central star. The mechanism driving the stellar mass loss has yet to be fully explained, but the rapid rotation of the central B star is believed to be crucial. Rapid rotation also produces gravity darkening, and we have now extended our disk models to include these effects. In this contribution, we focus on the effect of gravity darkening on the thermal structure of a circumstellar disk.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Collins, G. W. II 1966, ApJ 146, 914CrossRefGoogle Scholar
Porter, J. M. & Rivinius, T. 2003, PASP, 115, 1153CrossRefGoogle Scholar
Sigut, T. A. A. & Jones, C. E. 2007, ApJ, 668, 481CrossRefGoogle Scholar