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Turbulent motions in the interior of a star play an important role in itsevolution, since they transport chemical species, thermal energy and angularmomentum. Our overall goal is to construct a practical turbulent closure modelfor convective transport that can be used in a multi-dimensional stellarevolution calculation including the effects of rotation, shear and magneticfields. Here, we focus on the first step of this task: capturing the well-knowntransition from radiative heat transport to turbulent convection with andwithout rotation, as well as the asymptotic relationship between turbulent andradiative transport in the limit of large Rayleigh number. We extend theclosure model developed by Ogilvie (2003) and Garaud and Ogilvie (2005) toinclude heat transport and compare it with experimental results ofRayleigh-Benard convection.

A practical model of convective dynamics for stellar evolution calculations