Models of classical Be stars with gravity darkening

Details Models of classical Be stars with gravity darkening Models of classical Be stars with gravity darkening

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..272...95m&link_type=abstract

Active OB stars: structure, evolution, mass loss, and critical limits, Proceedings of the International Astronomical Union, IAU

Astronomy and Astrophysics

Astronomy

Stars: Emission-Line, Be, Circumstellar Matter, Stars: Rotation

Scientific paper

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.

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