Stellar mixing. I. Formalism

Details Stellar mixing. I. Formalism Stellar mixing. I. Formalism

Apr 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011a%26a...528a..76c&link_type=abstract

Astronomy & Astrophysics, Volume 528, id.A76

Astronomy and Astrophysics

Astrophysics

Turbulence, Diffusion, Convection, Hydrodynamics, Methods: Analytical, Stars: Rotation

Scientific paper

In this paper we use the Reynolds stress models (RSM) to derive algebraic expressions for the following variables: a) heat fluxes; b) μ fluxes; and c) momentum fluxes. These relations, which are fully 3D, include: 1) stable and unstable stratification, represented by the Brunt-Väisäla frequency, N2 = - gH_p-1 (nabla -nabla _ad)(1-R_μ); 2) double diffusion, salt-fingers, and semi-convection, represented by the density ratio Rμ = ∇μ(∇ - ∇ad)-1; 3) shear (differential rotation), represented by the mean squared shear Σ2 or by the Richardson number, Ri = N2Σ-2; 4) radiative losses represented by a Peclet number, Pe; 5) a complete analytical solution of the 1D version of the model. In general, the model requires the solution of two differential equations for the eddy kinetic energy K and its rate of dissipation, ɛ. In the local and stationary cases, when production equals dissipation, the model equations are all algebraic.
This work is dedicated to Aura Sofia Canuto.

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