Table of Contents
ISRN Astronomy and Astrophysics
Volume 2012, Article ID 987275, 10 pages
Research Article

On Estimating Fluxes due to Small-Scale Turbulent Convection in a Rotating Star

Institute of Astronomy & Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK

Received 30 November 2011; Accepted 15 January 2012

Academic Editors: R. Avila and S. Bogovalov

Copyright © 2012 D. O. Gough. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.


The way in which turbulent fluxes are usually represented in computations of large-scale flow in the convection zones of the sun and other stars is briefly described. A model of an ensemble of eddies that is capable of generalization to circumstances more complicated than the usual essentially spherically symmetrical convection zone is outlined. Generalization usually requires the introduction of new postulates, and, in so doing, also lays bare some of the assumptions, often implicit, in the usual mixing-length formalisms.