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Convective turbulent motions in the solar interior, as well as the mean flowsresulting from them, determine the evolution of the solar magnetic field. Withthe aim to get a better understanding of these flows we study anelasticrotating convection in a spherical shell whose stratification resembles that ofthe solar interior. This study is done through numerical simulations performedwith the EULAG code. Due to the numerical formulation, these simulations areknown as implicit large eddy simulations (ILES), since they intrinsicallycapture the contribution of, non-resolved, small scales at the same timemaximizing the effective Reynolds number. We reproduce some previous resultsand find a transition between buoyancy and rotation dominated regimes whichresults in anti-solar or solar like rotation patterns. Even thought therotation profiles are dominated by Taylor-Proudman columnar rotation, we areable to reproduce the tachocline and a low latitude near-surface shear layer.We find that simulations results depend on the grid resolution as a consequenceof a different sub-grid scale contribution.

Solar differential rotation: hints to reproduce a near-surface shear layer in global simulations