Convection is the main heat transport process in the liquid cores of planets and the primary energy source for planetary magnetic fields. These convective motions are thought to be turbulent and strongly constrained by rotation. In this talk, we will discuss the large-scale flows that form in this rapidly-rotating turbulent regime, which we explore with a combination of 2D and 3D numerical models. The convective motions consist of columnar vortices, which have a characteristic lengthscale depending solely on their speed and the rotation rate. We will describe how the large-scale dynamics can become dominated by intense jets, which impede the convective heat transport.

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