Left: evolution of the ratio, f_B between Ṁ_1,wind and the mass-loss rate without a magnetic field Ṁ_1,wind(B = 0) for spin-down and spin-up cases with differential (D) rotation, tidal forces (T) and wind magnetic braking (MB). Right: evolution of the separation, expressed in units of solar radii, for spin-down and spin-up cases with both solid (S) body and differential (D) rotation as a function of the spin angular velocity of the primary normalized to the orbital angular velocity. Point A denotes the ZAMS. Tidal torques dominate the orbital evolution from point A to point B in both spin-down and spin-up cases (τ_tides<τ_mb). At point B, one has that τ_tides = τ_mb The loss of mass due to stellar winds governs the orbital evolution from point B to point C in spin-down cases (τ_tides>τ_mb). The wind torques (or magnetic torques) are counteracted by tidal torques from point C to D in spin-down cases and from point B to D in spin-up cases. Point D denotes the beginning of Roche lobe overflow. The red and the green curves show the cases where the redistribution of angular momentum inside the star is due to shear instabilities and meridional currents (cases noted D in the box). The blue and the black curves are cases of solid body rotation (cases noted S in the box) R_sun is the solar radius. The dashed vertical lines correspond to perfect synchronization (Ω = ω_orb, magenta line) and to 90% and 110% of the orbital velocity (black lines left and right of magenta line, respectively).