The dynamo equation is solved for the solar convection zone withthe given ("observed") rotation law and positive α-effect. If thelatter exists in the entire convection zone the resulting dynamo showsstrong toroidal field belts in the polar region migrating equatorwards. Thesame happens for α concentrated at the bottom of the convection zonebut then we get too many belts with higher amplitude. The cycle period isalways too short. Including meridional circulation which is directed equatorwards at thebottom of the convection zone (where the eddy diffusivity is reduced), the amplitude of the toroidal field grows and the butterfly diagram reacheslow-latitudes. The cycle time approaches the solar value. The dynamo regime is highly sensitive to the interplay between flow anddiffusivity at the bottom of the convection zone. Stationary solutions arenot very seldom. For less active stars a slight increase of the cycle period with the rotation period is observed in agreement with the decrease of the meridional flow for faster rotation.