  The mean-field dynamo model is employed to study the non-linear dynamo
regimes in a fully convective star of mass 0.3$M_{\odot}$ rotating with period
of 10 days. For the intermediate value of the parameter of the turbulent
magnetic Prandl number, $Pm_{T}=3$ we found the oscillating dynamo regimes with
period about 40Yr. The higher $Pm_{T}$ results to longer dynamo periods. If the
large-scale flows is fixed we find that the dynamo transits from axisymmetric
to non-axisymmetric regimes for the overcritical parameter of the
$\alpha$effect. The change of dynamo regime occurs because of the
non-axisymmetric non-linear $\alpha$-effect. The situation persists in the
fully non-linear dynamo models with regards of the magnetic feedback on the
angular momentum balance and the heat transport in the star. It is found that
the large-scale magnetic field quenches the latitudinal shear in the bulk of
the star. However, the strong radial shear operates in the subsurface layer of
the star. In the nonlinear case the profile of the angular velocity inside the
star become close to the spherical surfaces. This supports the equator-ward
migration of the axisymmetric magnetic field dynamo waves. It was found that,
the magnetic configuration of the star dominates by the regular
non-axisymmetric mode m=1, forming Yin Yang magnetic polarity pattern with the
strong (>500 G) poloidal magnetic field in polar regions.
