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The paper presents a study of kinematic axisymmetric mean-field dynamo modelsfor a case of the meridional circulation with a deep-seated stagnation pointand a strong return flow at the bottom of the convection zone. This kind ofcirculation follows from mean-field models of the angular momentum balance inthe solar convection zone. We show that it is possible for this types ofmeridional circulation to construct kinematic dynamo models that resemble insome aspects the sunspot magnetic activity cycle. The dynamo model includesturbulent sources of the large-scale poloidal magnetic field production, due tokinetic helicity and a combined effect due to Coriolis force and thelarge-scale current. In these models the toroidal magnetic field, which isresponsible for the sunspot production, is concentrated at the bottom of theconvection zone, and is transported to low-latitude regions by the meridionalflow. The meridional component of the poloidal field is also concentrated atthe bottom of the convection zone while the radial component is concentrated innear polar regions. There are some issues which, perhaps, are resulted from thegiven meridional circulation pattern and the distribution of the magneticdiffusivity inside convection zone. In particular, in the near-equatorialregions the phase relations between the toroidal and poloidal componentsdisagree with observations. Also, we show that the period of the magnetic cyclemay not always monotonically decrease with the increase of the meridional flowspeed. Thus, for the further progress it is important to determine thestructure of the meridional circulation, which is one of the criticalproperties, from helioseismology observations.

Mean-field solar dynamo models with strong meridional flow at the bottom of the convection zone