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Rotation in Close Binaries

Published online by Cambridge University Press:  14 August 2015

R. Rajamohan  and
P. Venkatakrishnan
R. Rajamohan
Affiliation:
Indian Institute of Astrophysics Bangalore-560034 India
P. Venkatakrishnan
Affiliation:
Indian Institute of Astrophysics Bangalore-560034 India

Abstract

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It has been demonstrated (Zahn 1966 a, b, c; 1975, 1977) that turbulent viscous dissipation of tides can brake the rotation of stars having convective envelopes, while radiative dissipation can do like-wise for those having radiative envelopes. The time scales for the former are very small whereas those for the latter depend sensitively on the ratio r/R where r is the radius of the star and R, the binary separation. For most systems these turn out to be much less than their main sequence lifetimes. This fact affords a natural explanation for the preponderance of synchronous systems.

Type
I. General Reviews and Surveys
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 27 - 30
Copyright
Copyright © Reidel 1980 

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