The ice giant planets, Uranus and Neptune, have magnetic fields, atmospheric circulation patterns, and thermal emissions that are distinct from other planets in our Solar System. However, no self-consistent dynamical model has been able to reproduce all of these observations. We hypothesize that the dynamos and surface winds are dynamically coupled and argue that their characteristics are a consequence of three-dimensional turbulence that may be excited in planetary-scale water layers. Here we present dynamo models with thick and thin spherical shell geometries consistent with the range of possible internal structures of Uranus and Neptune. The style of convection is chosen a priori to yield small-scale and disorganized turbulence. In agreement with ice giant observations, both simulations (i) generate multipolar magnetic fields by fluctuating dynamo action, (ii) produce zonal jets with retrograde flow at the equator through angular momentum mixing, and (iii) predict local equatorial peaks in internal heat fluxes due to equatorial upwellings induced primarily by Hadley-like circulation cells. Thus, we argue that three-dimensional convective turbulence can explain the first-order geophysical observations of the ice giants. © 2013 Elsevier Inc.

An accurate description of turbulent core convection is necessary in order to build robust models of planetary core processes. Towards this end, we focus here on the physics of rapidly rotating convection. In particular, we present a closely coupled suite of advanced asymptotically-reduced theoretical models, efficient Cartesian direct numerical simulations (DNS) and laboratory experiments. Good convergence is demonstrated between these three approaches, showing that a comprehensive understanding of the dynamics appears to be within reach in our simplified rotating convection system. The goal of this paper is to review these findings, and to discuss their possible implications for planetary cores dynamics.