We apply a model of dynamo-driven mass loss, magnetic braking, and tidal friction to the evolution of stars with cool convective envelopes; in particular, we apply it to binary stars where the combination of magnetic braking and tidal friction can cause angular momentum loss from the orbit . For the present we consider the simplification that only one component of a binary is subject to these nonconservative effects, but we emphasize the need in some circumstances to permit such effects in both components.The model is applied to examples of (1) the Sun, (2) BY Dra binaries, (3) Am binaries, (4) RS CVn binaries, (5) Algols, and (6) post-Algols. A number of problems regarding some of these systems appear to find a natural explanation in our model. There are indications from other systems that some coefficients in our model may vary by a factor of 2 or so from system to system; this may be a result of the chaotic nature of dynamo activity.
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Eggleton et al. (2002) studied this question.
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