Dynamo cycles on slow and fast rotating solar analogs

Using the non-linear mean-field dynamo models we calculate the magnetic cycle parameters, like the dynamo cycle period, the amplitude of the total magnetic energy, and the Poynting flux luminosity from the surface for the solar analogs with rotation periods of range from 1 to 30 days. In general, the models show a decrease in the magnetic cycle period with the decrease of the stellar rotation period. We find the non-monotonic variation of the dynamo period with the rotation rate. The models for the rotational periods less than 10 days show the non-stationary evolution with a slight increase in the primary dynamo period with the increase of the rotation rate. There is a dynamo saturation for the star rotating with a period of two days and less. The saturation of the magnetic activity parameters is accompanied by depression of the differential rotation.