(2016; PhD Thesis).

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   ![Latitudinal (top) and radial (bottom) variation of the radial (dashed lines) and latitudinal (solid lines) turbulent pumping velocity components taken at a depth of 0.8 $R_{\odot}$ (top plot) and at a colatitude $40^\circ$ (bottom plot). Radial turbulent pumping is negative (downward) in both hemispheres. Latitudinal turbulent pumping is equatorward throughout the convection zone in both the hemispheres.](fig3.eps "fig:")  
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Results
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To bring out the significance of the recent observations, we first consider a single cell, shallow meridional flow, confined only to the top 10% of the convection zone (Fig. 1, right-hemisphere). In the first scenario we seek to answer the following question: Can solar-like cycles be sustained through magnetic field dynamics completely confined to the top 10% of the Sun?

In these simulations initialized with antisymmetric toroidal field condition (with initial B $\sim$ 100 kG), we first allow magnetic flux tubes to buoyantly erupt from 0.90 $R_{\odot}$ (i.e., the depth to which the shallow flow is confined) when they exceed a buoyancy threshold of $10^4$ Gauss (G). In this case we find that the simulated fields fall and remain below this threshold (at all latitudes at 0.90 $R_{\odot}$) with no buoyant eruptions, implying 