Turbulent compressible convection with rotation. II. Mean Flows and differential rotation

摘要

The effects of rotation on turbulent, compressible convection within stellar envelopes are studied through three-dimensional numerical simulations conducted within a local f-plane model. this work seeks to understand the types of differential rotation that can be established in convective envelopes of stars like the Sun, for which recent helioseismic observations suggest an angular velocity profile with depth and latitude at variance with many theoretical predictions. This paper analyzes the produced than are responsible for the mean(horizontally averaged)zonal and meridional flows that are produced by convection influenced by Coriolis forces.