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Parameters of magnetic activity on the solar type stars depend on theproperties of the dynamo processes operating in stellar convection zones. Weapply nonlinear mean-field axisymmetric $\alpha^2\Omega$ dynamo models tocalculate of the magnetic cycle parameters, such as the dynamo cycle period,the total magnetic flux and the Poynting magnetic energy flux on the surface ofsolar analogs with the rotation periods from 15 to 30 days. The models takeinto account the principal nonlinear mechanisms of the large-scale dynamo, suchas the magnetic helicity conservation, magnetic buoyancy, and effects ofmagnetic forces on the angular momentum balance inside the convection zones.Also, we consider two types of the dynamo models. The distributed (D-type)models employ the standard alpha-effect distributed on the whole convectionzone. The "boundary" (B-type) models employ the non-local alpha- effect, whichis confined to the boundaries of the convection zone. Both the D- and B-typemodels show that the dynamo-generated magnetic flux increases with the increaseof the stellar rotation rate. {It is found that for the considered range of therotational periods} the magnetic helicity conservation is the most significanteffect for the nonlinear quenching of the dynamo. This quenching is moreefficient in the B-type than in the D-type dynamo models. The D-type dynamoreproduces the observed dependence of the cycle period on the rotation rate forthe Sun analogs. For the solar analog rotating with a period of 15 days we findnonlinear dynamo regimes with multiply cycles.

Dependence of magnetic cycle parameters on period of rotation in nonlinear solar-type dynamos