Authors: Nicholas Featherstone (Southwest Research Institute), Catherine Blume (Univ. Colorado Boulder), Maria Camisassa (Universitat Politècnica de Catalunya), J.R. Fuentes (Univ. Colorado Boulder), Bradley Hindman (Univ. Colorado Boulder), Lydia Korre (Univ. Colorado Boulder), Loren Matilsky (Univ. California Santa Cruz)

In recent years, models of the solar convection zone that are at once turbulent and differentially rotating in a manner analogous to the Sun have been surprisingly difficult to construct. Instead, a state of differential rotation is achieved in which rapidly-rotating poles are accompanied by a slowly-rotating equator. This situation, sometimes referred to as the convective conundrum, arises naturally from the unphysical link between model diffusivities and the thermal content of downwelling plumes. We present results from a new survey of 3-D simulations designed to disentangle these two aspects of the convection, allowing solar-like differential rotation to be reliably achieved even in regimes of extreme turbulence. In particular, we describe how the properties of mean flows and convective structure vary with respect to a singular control parameter, the convective Rossby number, in systems characterized by high degrees of turbulence and density stratification.