Turbulent thermal convection in a differentially rotating channel
Abstract
Differentially rotating disks of gases and solids occur in several astrophysical systems, in particular in the inner parts of protostellar nebulae, of which our own solar system is thought to be a relic. The objectives of this paper are to: (1) study localized turbulence in circumstances approximating those found in accretion disks using previously existing expertise in performing direct numerical simulation of turbulent, incompressible channel flows with low Reynolds numbers; (2) determine the limitations of such calculations; and (3) extend the type of numerical simulation (e.g., to include density and stratification and compressibility effects and to accommodate higher Reynolds numbers with subgrid scale modeling) so that the relevant physical effects are realistically captured.
 Publication:

Annual Research Briefs, 1989
 Pub Date:
 February 1990
 Bibcode:
 1990arb..nasa..247C
 Keywords:

 Accretion Disks;
 Channel Flow;
 Compressibility Effects;
 Free Convection;
 Low Reynolds Number;
 Solar System Evolution;
 Turbulence;
 Turbulent Flow;
 Astrophysics;
 Computerized Simulation;
 Incompressible Flow;
 Magnetohydrodynamics;
 Rotating Disks;
 Stratification;
 Fluid Mechanics and Heat Transfer