2014/12/31 by В. В. Пипин, V. V. Pipin · 1 citation
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Classical mechanics #Computational physics #Convection #Convection zone #Dynamo #Dynamo theory #Geomagnetism and Paleomagnetism Studies #Magnetic energy #Magnetic field #Magnetic flux #Magnetic helicity #Magnetization #Magnetohydrodynamics #Mechanics #Physics #Quantum mechanics #Solar and Space Plasma Dynamics #Solar dynamo #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stv1026
11 pages, 6 figures, accepted in MNRAS
arxiv created 2015/05/07 · arxiv updated 2015/05/08 · openalex publication_date 2015/06/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Parameters of magnetic activity on the solar-type stars depend on the properties of the dynamo processes operating in stellar convection zones. We apply non-linear mean-field axisymmetric 2 dynamo models to calculate of the magnetic cycle parameters, such as the dynamo cycle period, the total magnetic flux and the Poynting magnetic energy flux on the surface of solar analogues with the rotation periods from 15 to 30 d. The models take into account the principal non-linear mechanisms of the large-scale dynamo, such as the magnetic helicity conservation, magnetic buoyancy and effects of magnetic forces on the angular momentum balance inside the convection zones. Also, we consider two types of the dynamo models. The distributed (D-type) models employ the standard -effect distributed on the whole convection zone. The 'boundary' (B-type) models employ the non-local -effect, which is confined to the boundaries of the convection zone. Both the D-and B-type models show that the dynamo-generated magnetic flux increases with the increase of the stellar rotation rate. It is found that for the considered range of the rotational periods the magnetic helicity conservation is the most significant effect for the non-linear quenching of the dynamo. This quenching is 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 analogues. For the solar analogue rotating with a period of 15 d, we find non-linear dynamo regimes with multiply cycles.