decrease of the dynamo period with the decrease of the rotational period of the star. The period of magnetic cycles changes from about 11 years for the solar case to the value which is about 3 year for the star rotating with the period about 15 days. The opposite tendency is found for the B-types dynamo models, where the dynamo period increases from 11 to 17 years when the rotational period decreases.

[The Table 2 gives results for the mean Poynting magnetic energy flux from the subsurface shear layer, $S_M$, for the D-type models. In the model we use the special boundary conditions, the Eq.(5) which allow the penetration of the toroidal field to the surface. In the linear case, this condition gives $S_M\sim B_s^2$, where $B_{s}$ is the toroidal magnetic field strength in the near-surface layer. In simulations it is found that the increase of the $S_M$ is gradually slow down when the rotation rates increase. Thus we can conclude that in the nonlinear dynamo the generated Poynting flux increases as $S_M\sim B_{s}^{2-\delta}$ where the $0 <\delta<1$.]{} This was predicted by (cf., to @2015MNRAS.446L..51B) for the dynamo models with magnetic helicity conservation as the principal dynamo non-linearity. It is 