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Energy Balance in Circumstellar Envelopes

Published online by Cambridge University Press:  12 April 2016

C. E. Millar ,
J. M. Marlborough  and
T. A. A. Sigut
C. E. Millar
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, CanadaN6K 3K7
J. M. Marlborough
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, CanadaN6K 3K7
T. A. A. Sigut
Affiliation:
Department of Physics and Astronomy, The University of Western Ontario, London, Ontario, CanadaN6K 3K7

Abstract

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We have successfully determined the kinetic temperature of the electron gas as a function of position in the circumstellar envelopes of Be stars. Our method yields a self-consistent solution of the equation for energy conservation, thus eliminating the necessity to assume arbitrarily a temperature for the gas. Our technique has been applied to Be stars of differing spectral classes, and we have also used several models for the distribution of the circumstellar material. The observed shape and relative line strength of the Hα line for several Be stars were matched successfully with these models. Recently we have begun to investigate the role of the diffuse radiation field in the Lyman continuum using the on-the-spot approximation. As a preliminary step to including metallic line cooling by the circumstellar gas, we have determined iron ionization fractions throughout the disks of both an early-type and a late-type Be star.

Type
6. Disks
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 597 - 602
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Apparao, K.M.V., Tarafdar, S.P. 1987, ApJ 322, 976 CrossRefGoogle Scholar
Ashok, N.M., Bhatt, H.C., Kulkami, P.V., Joshi, S.C. 1984, MNRAS 211, 471 CrossRefGoogle Scholar
Hony, S., Waters, L.B.F.M., Zaal, P.A., de Koter, A., Marlborough, J.M., Millar, C.E., Trams, N., Morris, P.W., de Graauw, T. 1999, A&A in pressGoogle Scholar
Marlborough, J.M., & Cowley, A.R. 1974, ApJ 187, 99 CrossRefGoogle Scholar
Millar, C.E., & Marlborough, J.M. 1999a, ApJ, in pressGoogle Scholar
Millar, C.E., & Marlborough, J.M. 1999b, ApJ 516, 276 CrossRefGoogle Scholar
Millar, C.E., & Marlborough, J.M. 1999c, ApJ 516, 280 Google Scholar
Millar, C.E., & Marlborough, J.M. 1998, ApJ 494, 715 CrossRefGoogle Scholar
Millar, C.E., Sigut, T.A.A., Marlborough, J.M. 1999, MNRAS, in pressGoogle Scholar
Osterbrock, D.E., 1974, Astrophysics of Gaseous Nebulae (USA: W.H. Freeman and Company)Google Scholar
Poeckert, R., & Marlborough, J.M. 1978, ApJ 220, 940 CrossRefGoogle Scholar
Waters, L.B.F.M., Coté, J., Lamers, H.J.G.L.M. 1987, A&A 185, 206 Google Scholar