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.](fig4b.eps "fig:")  
                                                                                                                                                                                                                                             (c)                                                                                                                                                                                                                                        
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   ![Dynamo simulations considering both shallow meridional flow and turbulent pumping but initialized with symmetric initial condition (quadrupolar state). Top panel shows the phase relationship between toroidal and poloidal field while bottom panel shows the butterfly diagram taken at the base of the convection zone ($0.71 R_\odot$).](fig5.eps "fig:")  
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We now introduce both radial and latitudinal turbulent pumping in our dynamo model to explore whether a Babcock Leighton flux transport dynamo can operate with meridional flow which is much shallower than previously assumed; we also extend this study to the scenario where meridional flow is altogether absent.

The turbulent pumping profile is determined from independent MHD simulations of solar magnetoconvection [@ossen02; @kapla06]. Profiles for radial and latitudinal turbulent pumping ($\gamma_r$ and $\gamma_\theta$) are: $$\begin{aligned}
\gamma_r = -  \gamma_{0r} \left[ 1 + \rm{erf}\left( \frac{r - 0.715R_\odot}{0.015R_\odot}\right) \right] \left[ 1 - \rm{erf} \left( \frac{r-0.97R_\odot}{0.1R_\odot}\right) \right] \nonumber \\
\times \left[ \rm{exp}\left( \frac{r-0.715R_\odot}{0.25R_\odot}\right) ^2 \rm{cos}\theta +1\right] ~~~~\end{aligned}$$ $$\begin{aligned}
