more efficient in the B-type than in the D-type dynamo models. The D-type dynamo reproduces the observed dependence of the cycle period on the rotation rate for the Sun analogs. For the solar analog rotating with a period of 15 days we find nonlinear dynamo regimes with multiply cycles.'
author:
- |
    V.V. Pipin [^1]\
    [Institute of Solar-Terrestrial Physics, Russian Academy of Sciences, Irkutsk, 664033, Russia]{}\
title: 'Dependence of magnetic cycle parameters on period of rotation in nonlinear solar-type dynamos'
---

=1

\[firstpage\]

stars:activity; stars:magnetic fields; dynamo: turbulence - magnetic fields

Introduction
============

Currently, there is an extensive database of observations of magnetic activity on the main sequence stars (see, e.g., reviews by @2009ARAA_donat [@lrsp-2012-1]). Cool stars with outer convective envelope are of particular interests because they are Sun-like. It is believed that the magnetic activity on the solar-like stars results from large-scale dynamo processes driven by turbulent convection and rotation [@2005PhR...417....1B]. Observations (e.g., [@2007ApJ_bohm; @2009ARAA_donat; @2010NewAstkazova; @2011IAUS_saar; @2013GeAe_kazova; @2014MNRAS_mars; @vid14MNR]), as well as the 2D mean-field models of the angular momentum balance and the 3D numerical simulations ) show that parameters of the differential rotation and convection, e.g., the typical size and turnover time of convective flows, depend on 