shows the &lt;&lt;long-term&gt;&gt; variations with period about 5-6 of the basic periods. [ The long-term variations are damped by the nonlinear $\Lambda$- quenching effects and the large-scale Lorentz forces. It seems that the model D3 (with the rotational period 14.5 days) is near the threshold of the nonlinear regime with the &lt;&lt;long-term&gt;&gt; variations.]{} This question should be studied further.

![image](Fig6){width=".8\textwidth"}

Figure 7 illustrates our findings about dependence of the magnetic cycles parameters, such as the magnitude of the total magnetic flux and the dynamo period, on the period of rotation of the star. [ The models D1 and D3 have the weaker dynamo than the models D0 and D2. The model with the non-local $\alpha$ effect, the B0, has the strongest toroidal field for the set of our dynamo models. Surprisingly, that the amplitude of the toroidal magnetic flux in the models B1 and B3 is rather similar to the models D1 and D3. This tells us that the magnetic buoyancy quenches the B-types dynamo models in a more efficient way than for the D-type. Also, the total magnetic flux in the fully nonlinear B-type model is about factor 3 smaller than in the D-type.]{}

The D-type models shows the 