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The Pattern of Convection in the Sun

Published online by Cambridge University Press:  14 August 2015

N. O. Weiss
N. O. Weiss*
Affiliation:
Dept. of Applied Mathematics and Theoretical Physics, University of Cambridge, England

Abstract

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The structure of solar magnetic fields is dominated by the effects of convection, which should be incorporated in any model of the solar cycle. Although mixing length theory is adequate for calculating the structure of main sequence stars, a better description of convection is needed for any detailed dynamo model. Recent work on nonlinear convection at low Prandtl numbers is reviewed. There has been some progress towards a theory of compressible convection, though there is still no firm theoretical evidence for cells with scales less than the depth of the converting layer. However, it remains likely that the pattern of solar convection is dominated by granules, supergranules and giant cells. The effects of rotation on these cells are briefly considered.

Type
Part 2: Solar Convection and Differential Rotation
Information
Symposium - International Astronomical Union , Volume 71: Basic Mechanisms of Solar Activity , 1976 , pp. 229 - 242
Copyright
Copyright © Reidel 1976 

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