erupt from 0.71 $R_{\odot}$, i.e. from base of the convection zone. In this case we get periodic solutions but analysis of the butterfly diagrams (taken both at the base of SCZ and near solar surface) shows that the toroidal field belts have almost symmetrical poleward and equatorward branches with no significant equatorward migration (see Fig. 2). Moreover, as already noted by Guerrero, G. & de Gouveia Dal Pino (2008), the solutions with shallow meridional flow always display quadrupolar parity in contradiction with solar cycle observations. Clearly, a shallow flow poses a serious problem for solar cycle models.

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   ![Dynamo simulations with shallow meridional flow but with radial and latitudinal turbulent pumping included (same convention is followed as in Fig. 2). The toroidal (a) and poloidal field (b) plots at a phase corresponding to cycle maxima show the dipolar nature of the solutions, and the butterfly diagram at the base of the convection zone ($0.71 R_\odot$) clearly indicates the equatorward propagation of the toroidal field that forms sunspots.](fig4a.eps "fig:")  
                                                                                                                                                                                                                  (a)                                               (b)                                                                                                                                                                                                                 
   ![Dynamo simulations with shallow meridional flow but with radial and latitudinal turbulent pumping included (same convention is followed as in Fig. 2). The toroidal (a) and poloidal field (b) 