Abstract
Abstract Thermal convection in deep planetary atmospheres or in planetary and stellar interiors is characterized by a finite angle between the vectors of rotation and gravity. This situation can be modelled in laboratory experiments through the use of centrifugal buoyancy. Earlier observations and recent measurements are reviewed and some new results are reported. Attention will be focused on experiments with a rotating cylindrical annulus and with rotating half-spheres. In some respects measurements and predictions of linear theory are in reasonable agreement; in other respects discrepancies exist. The observed transitions to a subharmonic frequency and to an aperiodic time dependence have not yet been understood on the basis of available non-linear theoretical models.
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