Mass and angular momentum loss of the Sun by magnetically driven winds

We reconstruct the evolution of the Sun's angular momentum and surface rotation starting from the stages immediately prior the ZAMS, in which a state of uniform rotation is assumed, to the present evolutionary stages, and compare the results with the surface rotational rates of stars with the same mass as the Sun in earlier evolutionary stages and with the present angular momentum of the Sun as deduced from helioseismology. We assume that the angular momentum loss is caused by the action of an external torque produced by a mass loss driven by a dynamo generated magnetic field, and that a mechanism, probably magnetic in origin, is able to transfer effectively angular momentum from the central regions to the surface where it is lost in the solar wind. Integration of the relevant equations for mass and angular momentum evolution indicates that the results are consistent with observations.