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Models of classical Be stars with gravity darkening

Published online by Cambridge University Press:  12 July 2011

Meghan A. McGill ,
T. A. Aaron. Sigut  and
Carol E. Jones
Meghan A. McGill
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: mmcgill8@uwo.ca, asigut@uwo.ca, cejones@uwo.ca
T. A. Aaron. Sigut
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: mmcgill8@uwo.ca, asigut@uwo.ca, cejones@uwo.ca
Carol E. Jones
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, Canada, N6A 3K7 emails: mmcgill8@uwo.ca, asigut@uwo.ca, cejones@uwo.ca
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Abstract

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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.

Keywords

stars: emission-lineBecircumstellar matterstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 95 - 96
Copyright
Copyright © International Astronomical Union 2011

References

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Sigut, T. A. A. & Jones, C. E. 2007, ApJ, 668, 481CrossRefGoogle Scholar