SIMBAD references

The mean-field dynamo model is employed to study the non-linear dynamo regimes in a fully convective star of mass 0.3 M_☉ rotating with period of 10 d. For intermediate value of parameter of the turbulent magnetic Prandl number, Pm_T = 3, we found the oscillating dynamo regimes with period about 40 yr. 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 α-effect. The change of dynamo regime occurs because of the non-axisymmetric non-linear α-effect. The situation persists in the fully non-linear dynamo models with regards for 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 non-linear 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. As a result of the differential rotation, it forms the Yin Yang magnetic polarity pattern with the strong (>500 G) poloidal magnetic field in polar regions.