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We present the results of three-dimensional simulations of the deepconvective envelope of a young (10 Myr) one-solar-mass star, obtained with theAnelastic Spherical Harmonic code. Since young stars are known to be fasterrotators than their main sequence counterparts, we have systematically studiedthe impact of the stellar rotation speed, by considering stars spinning up tofive times as fast as the Sun. The aim of these nonlinear models is tounderstand the complex interactions between convection and rotation. We discussthe influence of the turbulence level and of the rotation rate on the intensityand the topology of the mean flows. For all of the computed models, we find asolar-type superficial differential rotation, with an equatorial acceleration,and meridional circulation that exhibits a multicellular structure. Even if thedifferential rotation contrast decreases only marginally for high rotationrates, the meridional circulation intensity clearly weakens according to oursimulations. We have also shown that, for Taylor numbers above a certainthreshold (Ta>10^9), the convection can develop a vacillating behavior. Sincesimulations with high turbulence levels and rotation rates exhibit stronglycylindrical internal rotation profiles, we have considered the influence ofbaroclinic effects at the base of the convective envelope of these young Suns,to see whether such effect can modify the otherwise near cylindrical profilesto produce more conical, solar-like profiles.

Simulations of turbulent convection in rotating young solar-like stars: Differential rotation and meridional circulation