Natural Convection in Wide Spherical Shells

On a transitional and turbulent natural convection in spherical shells

Laminar and turbulent natural convection inside concentric spherical shells with isothermal cold and hot boundaries is numerically investigated up to Rayleigh number values Ra 6 10 and Pr = 0.71. The study utilizes direct numerical simulation (DNS), large eddy simulation (LES) and Reynolds averaged Navier– Stokes (RANS) approaches for investigation of the laminar, transitional and fully develop...

Convection in Rotating Spherical Fluid Shells

Convection driven by thermal buoyancy in rotating spherical bodies of fluid has long been recognized as a fundamental process in the understanding of the properties of planets and stars. Since these objects are rotating in general and since their evolution is associated with the transport of heat from their interiors convection influenced by the Coriolis force does indeed play a dominant role i...

Hydrothermal convection in moderately thin spherical shells.

Hydrothermal convection of pore water with a temperature-dependent viscosity within a permeable, internally heated, moderately thin spherical shell is investigated by both a perturbation analysis and a direct numerical simulation. The analysis and simulation are mainly focused on a thin spherical shell in that convective instabilities are characterized by the spherical harmonic degree l=6 with ...

“Unusual Properties of Convection and Dynamos in Rotating Spherical Shells”

Turbulent convection and differential rotation in spherical shells

Rotation is a general phenomenon in astrophysical systems on scales from planets to giant galaxy clusters. It is established during the formation of the system under gravitational compression. Typically the rotation rate is greatly enhanced during this process (Thompson et al. 2003). Rotation of stars defines their shapes and drives the internal circulation which redistributes chemical elements...