Abstract
The theory of the eddy diffusion of magnetic fields, momentum, and heat in rotating and magnetized fluids is reviewed. Rotation and magnetic fields both produce an anisotropy in the eddy diffusion and decrease the diffusivity values. Examples of the significance of anisotropy and quenching are given. Anisotropy results in a decline of the direction of travel of dynamo waves from the lines of constant angular velocity towards the equator. Magnetic quenching of the eddy diffusion is significant for the MHD equilibrium in sunspots. Attention is drawn to the fact that the formally defined diffusion tensors for rotating fluids contain the terms responsible for the generation of large-scale fields, in line with the true diffusion. A possible role of the correspondent generation effects in the solar dynamo is briefly discussed.
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Kitchatinov, L.L. (2003). Turbulent Transport in Rotating and Magnetized Fluids. In: Erdélyi, R., Petrovay, K., Roberts, B., Aschwanden, M. (eds) Turbulence, Waves and Instabilities in the Solar Plasma. NATO Science Series II: Mathematics, Physics and Chemistry, vol 124. Springer, Dordrecht. https://doi.org/10.1007/978-94-007-1063-4_5
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