Numerical solutions are evaluated of the equations governing the large-scale motions of rotating stellar convection zones, as derived by Durney and Spruit (DS). With the solar convection zone in mind, these equations were solved by a perturbation method with the uniformly rotating convection zone as the unperturbed state (approximated by a polytrope). The horizontal dimensions of the dominant convective eddy were assumed to be equal (l/sub theta/ = l/sub phi/) and the ratio l/sub theta//l/sub r/ ( = s) a constant independent of polar angle theta and radial distance r (phi is longitude; we recall that the ratios l/sub r//l/sub theta/, l/sub r//l/sub phi/, together with the mixing length, are the basic arbitrary parameters in the equations derived by DS). The collocation method was used to transform the set of partial differential equations in r and theta, into a set of ordinary differential equations in r which were then solved for a variety of boundary conditions. The solutions were evaluated for increasingly larger values of the angular velocity ..cap omega../sub 0/. For values of ..cap omega../sub 0/ smaller than the solar angular velocity the energy carried by the meridional motions was large enough to stabilize the turbulent convection, and solutionsmore » to the equations ceased to exist (we neglected in this paper the energy carried by radiation). Large pole-equator differences in flux were present in the lower part of the convection zone; at the surface, however, these pole-equator differences in flux were negligible.« less