Turbulent viscosity, magnetic diffusivity, and heat conductivity under the influence of rotation and magnetic field

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Abstract
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. An example of application of the theory to the global stellar circulation model is given and the implications for cosmic dynamos are briefly discussed.