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Simulating the Solar Dynamo

Published online by Cambridge University Press:  19 July 2016

Axel Brandenburg
Axel Brandenburg*
Affiliation:
HAO/NCAR∗ P.O. Box 3000, Boulder, CO 80307, USA

Abstract

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Mean-field and direct simulations of the hydrodynamics and hydromagnetics of the solar convection zone are discussed with the ultimate aim to understand the generation of differential rotation and magnetic fields. Various arguments constraining the values of the various turbulent diffusion coefficients are presented. It is suggested that the turbulent magnetic diffusivity is much smaller than the eddy viscosity which, in turn, is by up to a factor of ten smaller than the eddy conductivity. The magnetic field obtained from direct simulations is highly intermittent, and there is no clear systematic orientation of bipolar regions emerging from the convection zone. Various mechanisms that might cause such a field orientation are considered. Finally, the application of direct simulations to the determination of mean-field transport coefficients is emphasised.

Keywords

Solar dynamomean-field dynamodirect simulation
Type
3. Numerical Simulations of Convection and Dynamo Processes
Information
Symposium - International Astronomical Union , Volume 157: The Cosmic Dynamo , 1993 , pp. 111 - 121
Copyright
Copyright © Kluwer 1993 

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