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Stellar Convection as a Low Prandtl Number Flow

Published online by Cambridge University Press:  12 April 2016

Josep M. Massaguer
Josep M. Massaguer*
Affiliation:
Departament de Física Aplicada Universitat Politècnica de Catalunya, 08034 Barcelona, Spain

Abstract

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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
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 57 - 61
Copyright
Copyright © Springer-Verlag 1991

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