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Ionization Structure and Mass Loss for Rapidly-Rotating Near Main-Sequence B Stars

Published online by Cambridge University Press:  12 April 2016

J.E. Bjorkman  and
B.P. Abbott
J.E. Bjorkman
Affiliation:
Ritter Observatory, Dept. of Physics & Astronomy, University of Toledo, Toledo, OH 43606-3390, USA
B.P. Abbott
Affiliation:
Ritter Observatory, Dept. of Physics & Astronomy, University of Toledo, Toledo, OH 43606-3390, USA

Abstract

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Using the wind-compressed disk model to determine the density and velocity of a rapidly rotating wind, we calculate the 2-D ionization structure and corresponding line profiles. We find that previous estimates of the mass-loss rate based on spherically symmetric models may be a factor of 5–10 too small.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 632 - 635
Copyright
Copyright © Astronomical Society of the Pacific 2000

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