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Stellar Convection as a Low Prandtl Number Flow
Published online by Cambridge University Press: 12 April 2016
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
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- Copyright © Springer-Verlag 1991
References
Canuto, V.M., Cheng, Y., Hartke, G.J., Schilling, O., Chasnov, J.: 1990, J. Fluid Mech. (to be published)Google Scholar
Castaing, B., Gunaratne, G., Heslot, F.L., Kadanoff, L., Libchaber, A., Thomae, S., Wu, X.Z., Zaleski, S., Zanetti, G.: 1989, J. Fluid Mech.
204, 1
Google Scholar
Launder, B.E.: 1978, in “Turbulence”, ed. Bradshaw, P., p. 231, Topics in Applied Physics
12, Springer
Google Scholar
Massaguer, J.M.: 1990, in “Inside the Sun”, eds. Berthomieu, G. and Cribier, M. p. 101, Kluwer.Google Scholar
Spiegel, E.A.: 1962, in “Mécanique de la Turbulence”, Colloques Internationaux du CNRS à Marseille (Editions CNRS Paris), p. 181
Google Scholar
Toomre, J., Brummell, N., Cattaneo, F., Hurlburt, N.E.: 1990, Computer Phys. Commun.
59, 105
Google Scholar
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