Non-Boussinesq Low-Prandtl-number Convection with a Temperature-dependent Thermal Diffusivity

In an attempt to understand the role of the strong radial dependence of thermal diffusivity on the properties of convection in Sun-like stars, we mimic that effect in non-Oberbeck-Boussinesq convection in a horizontally extended rectangular domain (aspect ratio 16) by allowing the thermal diffusivity kappa to increase with the temperature (as in the case of stars). Direct numerical simulations (i.e., numerical solutions of the governing equations by resolving up to the smallest scales without requiring any modeling) show that, in comparison with Oberbeck-Boussinesq simulations (two of which we perform for comparison purposes), the symmetry of the temperature field about the mid-horizontal plane is broken, whereas the velocity and heat flux profiles remain essentially symmetric. Our choice of kappa(T), which resembles the variation in stars, results in a temperature field that loses its fine structures toward the hotter part of the computational domain, but the characteristic large scale of the turbulent thermal superstructures, which are structures whose size is typically larger than the depth of the convection domain, continues to be largely independent of the depth.

Automated summary

The study explores the effects of thermal diffusivity on convection in Sun-like stars. Numerical simulations reveal the breaking of symmetry in the temperature field but the maintenance of symmetry in velocity and heat flux profiles. The temperature field loses fine structures towards hotter areas while maintaining large-scale turbulent thermal superstructures independent of depth.