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W UMa Stars and Angular Momentum Loss

Published online by Cambridge University Press:  14 August 2015

Osmi Vilhu  and
Timo Rahunen
Osmi Vilhu
Affiliation:
Observatory and Astrophysics Laboratory University of Helsinki, Finland
Timo Rahunen
Affiliation:
Observatory and Astrophysics Laboratory University of Helsinki, Finland

Extract

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The structure and evolution of W UMa stars is still unsolved although considerable progress has been achieved in recent years. Most theoretical studies are based on the common convective envelope model by Lucy (1968a,b), which almost satisfactorily explains the nearly equal minima of the light curves. All A-type (Wilson, 1978) and some W-type systems (Whelan et al., 1979) may contain an evolved primary. In this case stable models exist (Hazlehurst, 1970; Moss and Whelan, 1970). Computations performed for the subsequent evolution (Moss, 1971; Hazlehurst and Meyer-Hofmeister, 1973; Rahunen and Vilhu, 1977) show nuclear time scale evolution towards more extreme mass ratio, supplemented by possible thermal time scale oscillations.

Type
IX. Contact Binaries
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 491 - 494
Copyright
Copyright © Reidel 1980 

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