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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

References

Bjorkman, J.E., Cassinelli, J.P. 1993, ApJ 409, 429 CrossRefGoogle Scholar
Cohen, D.H., Cassinelli, J.P., MacFarlane, J.J. 1997, ApJ 487, 867 Google Scholar
MacFarlane, J.J., Cohen, D.H., Wang, P. 1994, ApJ 437, 351 Google Scholar
MacFarlane, J.J., et al. 1993, ApJ 419, 813 Google Scholar
Prinja, R.K. 1989, MNRAS 241, 721 Google Scholar
Snow, T.P. 1981, ApJ 251, 139 CrossRefGoogle Scholar