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A Model for Adiabatic Mass-loss

Published online by Cambridge University Press:  01 April 2008

Hongwei. Ge ,
R. F. Webbink  and
Z. Han
Hongwei. Ge
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China; email: hongwei.ge@gmail.com Graduate University of Chinese Academy of Sciences, Beijing 100039, China
R. F. Webbink
Affiliation:
Department of Astronomy, University of Illinois, 1002 W. Green St. Urbana, IL 61801, USA
Z. Han
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China; email: hongwei.ge@gmail.com
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Abstract

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We describe our work on the development and application of a stellar structure code to compute model sequences representing donor stars in interacting binaries subject to rapid (adiabatic) mass-loss. The donor star is assumed to remain in hydrostatic equilibrium, but no heat flow is allowed. These sequences can be used to define bifurcation sequences in close binary evolution, and to circumscribe possible survivors of common envelope evolution.

Keywords

stars: evolutionstars: interiorsstars: mass lossbinaries: close
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 419 - 420
Copyright
Copyright © International Astronomical Union 2008

References

Eggleton, P. P., 1971, MNRAS 151, 351CrossRefGoogle Scholar
Eggleton, P. P., 1972, MNRAS 156, 361CrossRefGoogle Scholar
Eggleton, P. P., 1973, MNRAS 163, 179CrossRefGoogle Scholar
Han, Z., Podsiadlowski, P., & Eggleton, P. P. 1994, MNRAS 270, 121CrossRefGoogle Scholar
Han, Z., Podsiadlowski, P., Maxted, P. F. L., Marsh, T. R., & Ivanova, N. 2002, MNRAS 336, 449CrossRefGoogle Scholar
Hjellming, M. S. 1989a, Space Sci. Revs 50, 155CrossRefGoogle Scholar
Hjellming, M. S. 1989b, Ph.D. Thesis, University of Illinois at Urbana-ChampaignGoogle Scholar
Hjellming, M. S. & Webbink, R. F. 1987, ApJ 318, 794CrossRefGoogle Scholar
Paxton, B. 2004, PASP 116, 699CrossRefGoogle Scholar
Pols, O. R., Tout, C. A., Eggleton, P. P., & Han, Z. 1995 MNRAS 274, 964CrossRefGoogle Scholar
Pols, O. R., Schröder, K.-P., Hurley, J. R., Tout, C. A., & Eggleton, P.P. 1998 MNRAS 298, 525CrossRefGoogle Scholar