Dynamics of stellar convection zones: The effect of rotation on the turbulent viscosity and conductivity

Journal Article · Sat Dec 15 04:00:00 EST 1979 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/157589· OSTI ID:5486015

Durney, B R; Spruit, H C

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.

• Research Organization: National Center for Atmospheric Research
• OSTI ID: 5486015
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 234:3; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CONTINUITY EQUATIONS
CONVECTION
DIFFERENTIAL EQUATIONS
DISTRIBUTION FUNCTIONS
EQUATIONS
FLUID FLOW
HEAT FLUX
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
MOTION
PHYSICAL PROPERTIES
REYNOLDS NUMBER
ROTATION
STAR MODELS
STARS
SUN
TENSORS
THERMAL CONDUCTIVITY
THERMODYNAMIC PROPERTIES
TURBULENCE
VISCOSITY