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Massive stars with solar metallicity lose important amounts of rotationalangular momentum through their winds. When a magnetic field is present at thesurface of a star, efficient angular momentum losses can still be achieved evenwhen the mass-loss rate is very modest, at lower metallicities, or forlower-initial-mass stars. In a close binary system, the effect of wind magneticbraking also interacts with the influence of tides, resulting in a complexevolution of rotation. We study the interactions between the process of windmagnetic braking and tides in close binary systems. We discuss the evolution ofa 10 M$_\odot$ star in a close binary system with a 7 M$_\odot$ companion usingthe Geneva stellar evolution code. The initial orbital period is 1.2 days. The10 M$_\odot$ star has a surface magnetic field of 1 kG. Various initialrotations are considered. We use two different approaches for the internalangular momentum transport. In one of them, angular momentum is transported byshear and meridional currents. In the other, a strong internal magnetic fieldimposes nearly perfect solid-body rotation. The evolution of the primary iscomputed until the first mass-transfer episode occurs. The cases of differentvalues for the magnetic fields and for various orbital periods and mass ratiosare briefly discussed. We show that, independently of the initial rotation rateof the primary and the efficiency of the internal angular momentum transport,the surface rotation of the primary will converge, in a time that is short withrespect to the main-sequence lifetime, towards a slowly evolving velocity thatis different from the synchronization velocity. (abridged).

Close binary evolution. III. Impact of tides, wind magnetic braking, and internal angular momentum transport