  At present, Babcock-Leighton flux transport solar dynamo models appear as the
most promising model for explaining diverse observational aspects of the
sunspot cycle. The success of these flux transport dynamo models is largely
dependent upon a single-cell meridional circulation with a deep equatorward
component at the base of the Sun's convection zone. However, recent
observations suggest that the meridional flow may in fact be very shallow
(confined to the top 10 % of the Sun) and more complex than previously thought.
Taken together these observations raise serious concerns on the validity of the
flux transport paradigm. By accounting for the turbulent pumping of magnetic
flux as evidenced in magnetohydrodynamic simulations of solar convection, we
demonstrate that flux transport dynamo models can generate solar-like magnetic
cycles even if the meridional flow is shallow. Solar-like periodic reversals is
recovered even when meridional circulation is altogether absent, however, in
this case the solar surface magnetic field dynamics does not extend all the way
to the polar regions. Very importantly, our results demonstrate that the
Parker-Yoshimura sign rule for dynamo wave propagation can be circumvented in
Babcock-Leighton dynamo models by the latitudinal component of turbulent
pumping -- which can generate equatorward propagating sunspot belts in the
absence of a deep, equatorward meridional flow. We also show that variations in
turbulent pumping coefficients can modulate the solar cycle amplitude and
periodicity. Our results suggest the viability of an alternate magnetic flux
transport paradigm -- mediated via turbulent pumping -- for sustaining
solar-stellar dynamo action.
