  Previous work on the angular momentum balance and meridional circulation of
the solar convective zone (SCZ) generally consists either of semi-analytic
approaches in which a simple turbulence model is adopted, or full direct
numerical simulation (DNS) of the hydrodynamics or magnetohydrodynamics (MHD).
In both instances the inclusion of magnetic fields has been troublesome. Also,
both approaches have had difficulty reproducing the known angular velocity
profile of the SCZ; this is the Taylor Number Puzzle.
  I discuss preliminary work in which I incorporate magnetic fields into a
viscoelastic turbulence model for the SCZ and apply this to the problem of
meridional circulation and angular momentum balance. I suggest that such an
approach may help solve the Taylor Number Puzzle of the SCZ and bring
theoretical predictions for the large-scale motion of the SCZ in line with
observations.
