models. The increase of the turbulent diffusivity of the magnetic helicity will produce the similar effects as the decrease of the $R_m$ (see [@hub-br12]). It is likely that the helicity loss is modulated by the magnetic activity, e.g., by modulation of the coronal activity. Thus, the realistic dynamo model have to capture the basic mechanisms of the magnetic helicity loss, e.g., by means of including the stellar corona in simulations (see, [@bl-br2003; @warn2011]).]{}

[ The D-type model was calibrated against the solar case. The eigenvalue analysis for the D-type models (see, Pipin 2012, and references therein) shows that variations of the free parameters, like the $C_{\delta}$ (the $\Omega\times J$ effect), the $C_v$ (stratification of the turbulent diffusivity) can produce a dynamo with steady and non-oscillating large-scale magnetic field. The changes from the oscillating to steady dynamo regimes with the increase of the rotation rates could happen in the D-type dynamo models for the range of the parameters $C_{\delta,v}$ different than we use in the paper. The nonlinear dynamo models in these cases should be studied separately.]{}

Discussion and conclusions
==========================

In the paper we have studied the nonlinear effects in the large-scale magnetic solar-type dynamo on the parameters of the 