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5 Modeling Solar Convection

The extreme parameter regimes which prevail in the solar interior are inaccessible to laboratory experiments. Although experiments can provide important insight into fundamental aspects of turbulence and dynamo processes, most of our current knowledge about large-scale dynamics in the Sun comes from numerical and theoretical modeling efforts. In this section we briefly describe some of the modeling strategies which have been used. A comprehensive account is beyond the scope of this review; the reader is referred to the publications cited in this section for more information. For further information on laboratory experiments regarding convection and dynamo processes in a solar/planetary context, the reader is referred to Hart et al. (1986), Siggia (1994), Niemela et al. (2000), Busse (2000Jump To The Next Citation Point), and Gailitis et al. (2002).


 5.1 The challenge
 5.2 3D numerical simulations
 5.3 Reduced models
 5.4 Thin-shell approximations for the tachocline

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