Â鶹ӰԺ

Rotating Rayleigh-Bénard convection is the canonical framework for investigating the fundamental dynamics of stars, planetary interiors, and terrestrial oceans.Ìý To understand these turbulent and rapidly rotating systems, several techniques are used to study them: asymptotic methods, direct numerical simulations of the Boussinesq equations (DNS) and experiments.Ìý While these methods show good quantitative agreement for stress free boundary conditions, the case of no-slip boundaries presents an interesting difference. Along the rigid boundaries, Ekman layers form which result in Ekman pumping. In this talk, I will present an asymptotically reduced PDE model for rotating, thermal convection that incorporates these Ekman layers and compare results from our simulations to those from DNS and experiments. The model is used to investigate the heat transport efficiency as well as the inverse cascade of energy in the geostrophic turbulence regime.

Ìý