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A Rotating, Magnetic, Radiation-Driven Wind Model Applied to Be Stars

Published online by Cambridge University Press:  23 September 2016

C. H. Poe  and
D. B. Friend
C. H. Poe
Affiliation:
Astronomy Department, University of Wisconsin, Madison, Wisconsin, 53706, USA
D. B. Friend
Affiliation:
Astronomy Department, University of Wisconsin, Madison, Wisconsin, 53706, USA

Extract

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With their rotating, magnetic, radiation-driven wind model, Friend & MacGregor (1984) found that rapid rotation and an open magnetic field could enhance the mass loss rate (ṁ) and terminal velocity (V∞) in an 0 star wind. The purpose of this paper is to see if this model could help explain the winds from Be stars. The following features of Be star winds need to be explained: 1) Be stars exhibit linear polarization (Coyne & McLean 1982), indicating an enhanced equatorial density. 2) There appears to be enhanced mass loss (at low velocity) in the equatorial plane, from IRAS observations of Waters (1986). 3) The width of the broad Balmer emission lines remains unexplained.

Type
IV. Models
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 437 - 439
Copyright
Copyright © Cambridge University Press 1987

References

Castor, J. I., Abbott, D. C. & Klein, R. I. (1975). Radiation-driven winds in Of stars. Ap. J., 195, 157-74.Google Scholar
Coyne, G. V. & McLean, I. S. (1982). Polarimetry and physics of Be star envelopes. In IAU Symposium 98, Be Stars, ed. Jaschek, M. & Groth, H.-G., pp. 77–93. Dordrecht: Reidel.Google Scholar
Friend, D. B. & MacGregor, K. B. (1984). Winds from rotating, magnetic, hot stars. I. general model results. Ap. J., 282, 591–602.Google Scholar
Poe, C. H. & Friend, D. B. (1986). A rotating, magnetic, radiation-driven wind model applied to Be stars. Ap. J., 311, in press.Google Scholar
Waters, L. B. F. M. (1986). The density structure of discs around Be stars derived from IRAS observations. Astr. Ap., in press.Google Scholar
Weber, E. J. & Davis, L. Jr. (1967). The angular momentum of the solar wind. Ap. J., 148, 217-27.CrossRefGoogle Scholar