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Colliding winds in O-type binaries

Published online by Cambridge University Press:  07 August 2017

Douglas R. Gies
Douglas R. Gies*
Affiliation:
Department of Physics and Astronomy Georgia State University, Atlanta, GA 30303-3083, U.S.A. I: gies@chara.gsu.edu

Abstract

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In close binary systems of O-type stars, the individual stellar winds will collide between the stars to form shock fronts. The existence of the shock region can be established through observations of excess X-ray emission and orbital phase-related variations in UV wind features and optical emission lines. Here I report on work in progress on the orbital variations of the UV wind lines in a large sample of O-binaries that have been observed with the International Ultraviolet Explorer satellite. In most of these binaries, the blue absorption trough of the P-Cygni lines weakens when the strong wind component is behind its companion, in accordance with expectations for colliding winds. I describe how the radial velocity variations of the wind features differ from the orbital motions. Finally I discuss observations of Hα emission in these systems, with emphasis on HD 47129 (Plaskett's star). Such optical emission lines act as a probe of high density regions in the winds.

Keywords

stars: O-type starswindsclose binaries
Type
Session VII - Hydrodynamics and high-energy physics of colliding winds
Information
Symposium - International Astronomical Union , Volume 163: Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution , 1995 , pp. 373 - 381
Copyright
Copyright © Kluwer 1995 

References

Bagnuolo, W.G., Gies, D.R., Wiggs, M.S. 1992, ApJ 385, 708 CrossRefGoogle Scholar
Chlebowski, T., Garmany, C.D. 1991, ApJ 368, 241 Google Scholar
Drechsel, H., Rahe, J., Kondo, Y., McCluskey, G.E. 1981, A&A 94, 285 Google Scholar
Friend, D.B., Castor, J.I. 1982, ApJ 261, 293 Google Scholar
Gies, D.R., Wiggs, M.S. 1991, ApJ 375, 321 Google Scholar
Gies, D.R., Wiggs, M.S., Bagnuolo, W.G. 1993, ApJ 403, 752 Google Scholar
Heap, S.R. 1981, in: Chapman, R.D. (ed.), The Universe at Ultraviolet Wavelengths: The First Two Years of IUE, NASA CP 2171 , p. 485 Google Scholar
Howarth, I.D., Stickland, D.J., Prinja, R.K., Koch, R.H., Pfeiffer, R.J. 1991, The Observatory 111, 167 Google Scholar
McCluskey, G.E., Kondo, Y. 1976, ApJ 208, 760 CrossRefGoogle Scholar
Sahade, J., Brandi, E. 1991, ApJ 379, 706 Google Scholar
Stevens, I.R. 1993, ApJ 404, 281 Google Scholar
Stevens, I.R., Blondin, J.M., Pollock, A.M.T. 1992, ApJ 386, 265 Google Scholar
Struve, O., Sahade, J., Huang, S.-S. 1958, ApJ 127, 148 Google Scholar
Struve, O., Sahade, J., Zebergs, V., Lynds, B.T. 1958, PASP 70, 267 CrossRefGoogle Scholar
Wiggs, M.S., Gies, D.R. 1992, ApJ 396, 238 Google Scholar
Wiggs, M.S., Gies, D.R. 1993, ApJ 407, 252 Google Scholar