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Stellar Convection as a Low Prandtl Number Flow
Published online by Cambridge University Press: 12 April 2016
Abstract
Thermal convection in the Sun and cool stars is often modeled with the assumption of an effective Prandtl number σ ≃ 1. Such a parameterization results in masking of the presence of internal shear layers which, for small σ, might control the large scale dynamics. In this paper we discuss the relevance of such layers in turbulent convection. Implications for heat transport – i.e. for the Nusselt number power law – are also discussed.
- Type
- Part I Convection and turbulence as the basis of magnetic activity
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- Copyright © Springer-Verlag 1991