On the dynamics of stellar convection zones - The effect of rotation on the turbulent viscosity and conductivity

Details On the dynamics of stellar convection zones - The effect of rotation on the turbulent viscosity and conductivity On the dynamics of stellar convection zones - The effect of rotation on the turbulent viscosity and conductivity

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...234.1067d&link_type=abstract

Astrophysical Journal, Part 1, vol. 234, Dec. 15, 1979, p. 1067-1078.

Astronomy and Astrophysics

Astrophysics

77

Convective Flow, Solar Rotation, Stellar Structure, Turbulent Heat Transfer, Adiabatic Flow, Reynolds Stress

Scientific paper

We derive expressions for the turbulent viscosity and turbulent conductivity applicable to convection zones of rotating stars. We assume that the relative dimensions of the dominant convective cell are known and derive a simple distribution function for the turbulent convective velocities under the influence of rotation. From this distribution function (which includes, in particular, the stabilizing effect of rotation on convection) we calculate in the mixing-length approximation: (i) the turbulent Reynolds stress tensor and (ii) the expression for the heat flux in terms of the superadiabatic gradient. The contributions of the turbulent convective motions to the mean momentum and energy equation (which determine the large-scale motions in stellar convection zones) are treated consistently, and assumptions about the turbulent viscosity and heat transport are replaced by assumptions about the turbulent flow itself. The free parameters in our formalism are the relative cell dimensions and their dependence on depth and latitude.

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