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The propagation of meridional circulation below the base of the convectionzone of low-mass stars may play a crucial role in the transport of angularmomentum and also significantly contribute to the transport of chemical speciesand magnetic fields within their stable radiative zone. We systematically studythese large-scale mean flows by performing three-dimensional (3D) globalnumerical simulations in a spherical shell that consists of a convection zone(CZ) overlying a stably stratified region. We find that the meridional flowscan penetrate distances as large as $\sim 0.21r_o$ (where $r_o$ is the outerradius) below the base of the convection zone, provided that theEddington-Sweet timescale $t_{ES}$ is much shorter than the viscous timescale$t_{\nu}$ as measured by the parameter $\sigma=(t_{ES}/t_{\nu})^{1/2}$. In thesolar-like regime where $\sigma\lesssim 1$ in the upper radiative zone (RZ), wefind that the angular momentum transport in the deep RZ is determined primarilyby the action of the Coriolis force on meridional flows. In contrast, in modelsrun in the $\sigma> 1$ regime, the meridional flows become weaker and theviscous effects dominate. We find that the penetration lengthscale$\delta_{MC}$ of these mean flows when $\sigma\lesssim 1$ is proportional to$\sigma^{-0.22}$. Our findings may provide a better understanding of the roleof the meridional flows in the dynamics of the solar interior and inform futurenumerical studies that are focused on capturing solar-like dynamicsself-consistently.

On the penetration of large-scale flows into stellar radiative zones