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The model of magnetic braking of solar rotation considered by Charbonneau &MacGregor (1993) has been modified so that it is able to reproduce for thefirst time the rotational evolution of both the fastest and slowest rotatorsamong solar-type stars in open clusters of different ages, without coming intoconflict with other observational constraints, such as the time evolution ofthe atmospheric Li abundance in solar twins and the thinness of the solartachocline. This new model assumes that rotation-driven turbulent diffusion,which is thought to amplify the viscosity and magnetic diffusivity in stellarradiative zones, is strongly anisotropic with the horizontal components of thetransport coefficients strongly dominating over those in the verticaldirection. Also taken into account is the poloidal field decay that helps toconfine the width of the tachocline at the solar age. The model's propertiesare investigated by numerically solving the azimuthal components of the coupledmomentum and magnetic induction equations in two dimensions using a finiteelement method

A Model of Magnetic Braking of Solar Rotation That Satisfies Observational Constraints