A numerical study on turbulent heat transfer in convective envelopes
Abstract
A twodimensional temperature equation is used to study the wellknown solar heatflux problem. A spherically symmetric heat flux may enter the convection zone at its bottom and leave following the StefanBoltzmann law. Meridional circulation is involved; radiation is still ignored. In order to establish the eddyconductivity tensor for the simplest rotating turbulences, a secondorder correlation approximation is used. The resulting poleequator differences vary for various profiles of eddy conductivity and turnover time. They prove to be small only for small stratification or strong outward decrease of turnover time. The fact that no latitudinally profiled mean temperature is observed might thus have to do with the real outward drop of the rotational influence on convection.
 Publication:

Astronomische Nachrichten
 Pub Date:
 1984
 DOI:
 10.1002/asna.2113050505
 Bibcode:
 1984AN....305..229A
 Keywords:

 Convective Heat Transfer;
 Heat Flux;
 Solar Flux;
 Stellar Envelopes;
 Turbulent Heat Transfer;
 Energy Transfer;
 Meridional Flow;
 Tensor Analysis;
 Thermal Conductivity;
 Vortices;
 Solar Physics