of the angular velocity for the stationary stage of the magnetic activity evolution.]{} The D2 and B3 models show the stronger deviation of the rotation profiles from the unperturbed state than the models D3 and B4. The magnetic helicity conservation quenches the amplitude of the torsional oscillations by means of damping the magnitude of the dynamo generated magnetic fields. For the D2 and B3 type models the distribution of the angular velocity deviates strongly from the radial-like profiles for the star rotating with the period of 14.5 days (see, e.g., Figure 4 (top,left). In the model D2 and B3 the rotation profiles in the mid part of the convection zone becomes more and more cylinder-like when the period of the rotation decreases. Figure 5 shows results for the surface differential rotation and the magnitude of the torsional oscillations in the dynamo modes D2, D3, B3 and B4. [The magnitude of the torsional oscillations is determined by the maximum amplitude of the zonal velocity perturbation at latitude of 30$^{\circ}$ north on the surface in the stationary state of evolution.]{}

We find that in the model D2 the magnetic activity reduces the latitudinal shear at the surface by 10% of the $\Delta\Omega_{\odot}$, 