Turbulent convection in a rotating body is a common but poorly understood phenomenon in astrophysical and geophysical settings. Consideration of boundary effects offers a fresh angle on this thorny problem. Heat energy is transported by three basic processes: conduction, radiation and convection. But which of them is likely to dominate in any given circumstance? In particular, how can we quantify the relative efficiency of each process, not least of convection, which is inherently nonlinear and turbulent? This problem is especially challenging for understanding the evolution and interior structure of stars and planets - a task that is further complicated by the fact that most stars and planets are rotating, which may modify the style of convection and influence its efficiency.
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