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The Masive Binary SV Centauri

Published online by Cambridge University Press:  07 August 2017

Albert P. Linnell
Albert P. Linnell*
Affiliation:
Department of Physics and Astronomy Michigan State University East Lansing, MI 48824

Abstract

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Current light synthesis models of SV Centauri require a highly overcontact system with an 8000K temperature discontinuity between components. Current evolutionary models support the overcontact status, and describe the system as in the final stage of rapid mass transfer prior to mass reversal, calculated to occur within 2500 years. Light synthesis simulation provides a poor fit to the observations, and requires an ad hoc assumption to fit the substantial O'Connell effect.

IUE spectra have been reported to indicate the presence of a 200 000K source of small dimensions in the system. New spectrum synthesis results demonstrate there is no hot spot, but there is extra radiation longwards of 200nm that is unaccounted for by the overcontact model.

Postulated presence of an accretion disk around the mass gainer prospectively overcomes the observational anomalies. Formation of the accretion disk apparently violates the Lubow-Shu criterion. A reasonable scenario nonetheless supports accretion disk formation. Conflict with the theoretical models can be resolved on the postulate that the spherical accretion assumed in those models render them inapplicable to this system.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 369 - 372
Copyright
Copyright © Kluwer 1992 

References

[1] Balbus, S.A., & Hawley, J.F. 1991, ApJ, 376, 214 CrossRefGoogle Scholar
[2] DeGreve, J.P. 1989, in IAU Colloquium 107, Algols, ed. Batten, A.H. (Dordrecht:Kluwer)Google Scholar
[3] Dreschel, H., Rahe, J., Wargau, W., & Wolf, B. 1982a, A&A, 110, 246 Google Scholar
[4] Dreschel, H., Rahe, J., & Wargau, W. 1982b, in IAU Colloquium 69, Binary and Multiple Stars as Tracers of Stellar Evolution, ed. Kopal, Z. & Rahe, J. (Dordrecht:Kluwer)Google Scholar
[5] Hawley, J.A., & Balbus, S.A. 1991, ApJ, 376, 223 CrossRefGoogle Scholar
[6] Hubeny, I., & Plavec, M.J. 1991, AJ, in press Google Scholar
[7] Linnell, A.P. 1991, ApJ, 379, in press Google Scholar
[8] Linnell, A.P., & Scheick, X. 1989, BAAS, 21, 1084 Google Scholar
[9] Livio, M. 1989, in IAU Colloquium 107, Algols, ed. Batten, A.H. (Dordrecht:Kluwer)Google Scholar
[10] Livio, M., Soker, N., & Dgani, R. 1986, ApJ, 305, 267 Google Scholar
[11] Lubow, S.H., & Shu, F.H., 1975, ApJ, 198, 383 Google Scholar
[12] Nakamura, M., & Nakamura, Y. 1982, Ap&SS, 83, 163 Google Scholar
[13] Nakamura, M., & Nakamura, Y. 1985, PASJ, 37, 545 Google Scholar
[14] Rucinski, S.M. 1976, PASP, 88, 244 Google Scholar
[15] Sybesma, C.H.B. 1986, A&A, 159, 108 Google Scholar
[16] Wilson, R.E., & Starr, T.C. 1976, MNRAS, 176, 625 Google Scholar