Example of DR profiles that emerge in numerical simulations of stellar convective envelopes. The top panels show DR profiles achieved in MHD models of B22, from high to low Rossby numbers (left to right). The bottom right profile is characteristic of low Rossby numbers in hydrodynamics models of Brun et al. (2017). The symmetric part of the surface velocity from these meridional cuts is illustrated in the bottom left panel for all profiles.