dynamo cycles for the range of the rotation periods from 14.5 to 30 days. This a preliminary study. The dynamo model lacks the self-consistent description of the angular momentum in the convection zone of a star. We also exclude the evolutionary changes of the stellar convection zone structure, which could occur together with the angular momentum loss. The model also lacks the effects of the meridional circulation to the dynamo action, which is found in the direct numerical simulations and it is extensively used in the advection B-type solar dynamo models [@raey]. Therefore I consider the results of the paper as preliminary.

We find that the D-type dynamo models (the dynamo distributed over the convection zone) satisfactory explains the dependence of the dynamo magnitude and the dynamo periods on the periods of rotation of the star (see, e.g., @soon94 [@2011IAUS_saar]). [These properties are expected from the qualitative predictions made for linear and weakly-nonlinear Parker-type dynamo models [@ku98]. For the Sun, the relation between the magnitude of the solar cycle and its period is a part of the Waldmeier’s relations [@w36].]{} The B-type models fails to explain the latter fact. In mean-field models of the stellar dynamo it was seen earlier 