Abstract
Convection in a frame of reference rotating rapidly about an axis perpendicular to the direction of gravity is a model system for convection in the equatorial region of gaseous planets and is realized in recent laboratory experiments. It is found that the transition from rotationally constrained two-dimensional to three-dimensional flows in this system does not occur at some fixed Rossby number. Instead, the Rossby number at the transition depends on the Reynolds number of the flow. The transition occurs when the Taylor columns which constitute the two-dimensional flow become unstable to elliptical instability.
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