Hostname: page-component-5db6c4db9b-wnbrb Total loading time: 0 Render date: 2023-03-24T09:29:08.529Z Has data issue: true Feature Flags: { "useRatesEcommerce": false } hasContentIssue true
  • English

Structure and evolution of W UMa-type systems

Published online by Cambridge University Press:  01 April 2008

Lifang Li ,
Fenghui Zhang ,
Zhanwen Han ,
Dengkai Jiang  and
Tianyu Jiang
Lifang Li
Affiliation:
National Astronomical Observatories Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan Province, 650011, P.R. China email: gssephd@public.km.yn.cn .or. llf@ynao.ac.cn
Fenghui Zhang
Affiliation:
National Astronomical Observatories Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan Province, 650011, P.R. China email: gssephd@public.km.yn.cn .or. llf@ynao.ac.cn
Zhanwen Han
Affiliation:
National Astronomical Observatories Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan Province, 650011, P.R. China email: gssephd@public.km.yn.cn .or. llf@ynao.ac.cn
Dengkai Jiang
Affiliation:
National Astronomical Observatories Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan Province, 650011, P.R. China email: gssephd@public.km.yn.cn .or. llf@ynao.ac.cn Graduate University of Chinese Academy Sciences, Beijing 100039, China
Tianyu Jiang
Affiliation:
National Astronomical Observatories Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming, Yunnan Province, 650011, P.R. China email: gssephd@public.km.yn.cn .or. llf@ynao.ac.cn Graduate University of Chinese Academy Sciences, Beijing 100039, China
Rights & Permissions[Opens in a new window]

Abstract

HTML view is not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We summarize and discuss our recent works on the structure and evolution of low-mass W UMa-type contact binary stars. Three conclusions are given as followings: (1) The energy transfer is taken place in the radiative region of common envelope of W UMa systems; (2) The magnetic activity level of W UMa systems is weaker than that of non-contact binaries or rapid-rotating single stars; (3) The evolutionary outcome of W UMa systems might be the rapid-rotating single stars, and an average lifetime is derived to be about 7 Gyr for W UMa systems.

Keywords

binaries: closestars: evolutionstars: rotationstars: activity
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. 423 - 424
Copyright
Copyright © International Astronomical Union 2008

References

Eggleton, P. P., 1971, MNRAS, 151, 351CrossRefGoogle Scholar
Eggleton, P. P. & Kiseleva-Eggleton, L., 2001, ApJ, 562, 1012CrossRefGoogle Scholar
Hurley, J. R., Tout, C. A., & Pols, O. R., 2002, MNRAS, 329, 897CrossRefGoogle Scholar
Kähler, H., 2002, A&A, 395, 899Google Scholar
Li, L., Han, Z., & Zhang, F., 2005, MNRAS, 351, 137CrossRefGoogle Scholar
Li, L., Han, Z. & Zhang, F., 2005, MNRAS, 360, 272CrossRefGoogle Scholar
Lucy, B., 1976, ApJ, 205, 208CrossRefGoogle Scholar
Robertson, J. A. & Eggleton, P. P., 1977, MNRAS, 179, 359CrossRefGoogle Scholar
Rucinski, S. M., 1992, AJ, 103, 960CrossRefGoogle Scholar
Stepień, K., Schmitt, H. M. M., & Voges, W., 2001, A& A, 370, 157Google Scholar
Yakut, K. & Eggleton, P. P., 2005, ApJ, 629, 1055CrossRefGoogle Scholar