Magnetic braking of G and K dwarfs without core-envelope decoupling

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Abstract
In the light of recent claims that conventional magnetic braking models cannot explain the rotational evolution of the rapidly rotating G dwarfs in the α Persei and Pleiades clusters, we re-examine the braking problem within the simple framework of the Weber-Davis model with thermo-centrifugal wind acceleration. We find that the braking efficiency required to follow the evolution of individual stars from the age of the Pleiades to the age of the Sun and beyond is consistent with present knowledge of the solar magnetic field strength, a simple linear dependence of the field strength on the inverse Rossby parameter, and a mass-loss rate that scales roughly as the square of the surface field strength. Dynamo saturation at 15 to 45 times the present solar rotation rate is required to explain the behaviour of the rapid rotators in the young clusters, but there is no need to invoke exotic angular momentum loss mechanisms or core-envelope decoupling.

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