  The meridional circulation of the Sun is observationally found to vary with
the solar cycle, becoming slower during the solar maxima. We explain this by
constructing a theoretical model in which the equation of the meridional
circulation (the $\phi$ component of the vorticity equation) is coupled with
the equations of the flux transport dynamo model. We find that the Lorentz
force of the dynamo-generated magnetic fields can slow down the \MC\ during the
solar maxima in broad conformity with the observations.

Solar and Stellar Astrophysics