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We study how tides in a binary system induce some specific internal shearmixing, able to substantially modify the evolution of close binaries prior tomass transfer. We construct numerical models accounting for tidal interactions,meridional circulation, transport of angular momentum, shears and horizontalturbulence and consider a variety of orbital periods and initial rotationvelocities. Depending on orbital periods and rotation velocities, tidal effectsmay spin down (spin down Case) or spin up (spin up Case) the axial rotation. Inboth cases, tides may induce a large internal differential rotation. Theresulting tidally induced shear mixing (TISM) is so efficient that the internaldistributions of angular velocity and chemical elements are greatly influenced.The evolutionary tracks are modified, and in both cases of spin down and spinup, large amounts of nitrogen can be transported to the stellar surfaces beforeany binary mass transfer. Meridional circulation, when properly treated as anadvection, always tends to counteract the tidal interaction, tending to spin upthe surface when it is braked down and vice versa. As a consequence, the timesneeded for the axial angular velocity to become equal to the orbital angularvelocity may be larger than given by typical synchronization timescales. Also,due to meridional circulation some differential rotation remains in tidallylocked binary systems.

Close binary evolution I. The tidally induced shear mixing in rotating binaries