The old problem of turbulent diffusion is addressed to define the influence of rotation and magnetic field -the usual ingredients of astrophysical bodies -on the effective transport coefficients. Either rotation and magnetism produce the anisotropy and quenching. The tensorial structures of the diffusivities and their dependences on the angular velocity and the field strength are explicitly defined. A n example of application of the theory to the global stellar circulation model is given and the implications for cosmic dynamos are briefly discussed.
We propose a solar dynamo model distributed in the bulk of the convection zone with toroidal magnetic-field flux concentrated in a near-surface layer. We show that if the boundary conditions at the top of the dynamo region allow the large-scale toroidal magnetic fields to penetrate close to the surface, then the modeled butterfly diagram for the toroidal magnetic field in the upper convection zone is formed by the subsurface rotational shear layer. The model is in agreement with observed properties of the magnetic solar cycle.
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