  We present axisymmetric simulations of the coupled convective and radiative
regions in the Sun in order to investigate the angular momentum evolution of
the radiative interior. Both hydrodynamic and magnetohydrodynamic models were
run. We find an initial rapid adjustment in which the dif- ferential rotation
of the convection zone viscously spreads into the radiative interior, thus
forming a "tachocline". In polar regions the subsequent spread of the
tachocline is halted by a counter-rotating meridional circulation cell which
develops in the tachocline. Near the equator such a counter-rotating cell is
more intermittent and the tachocline penetration depth continues to increase,
albeit more slowly than previously predicted. In the magnetic models we impose
a dipolar field initially confined to the radiative interior. The behavior of
the magnetic models is very similar to their non-magnetic counter- parts.
Despite being connected to the convection zone, very little angular momentum is
transferred between the convective and radiative regions. Therefore, while it
appears that a magnetic field is not necessary to stop the tachocline spread,
it also does not promote such a spread if connected to the convection zone.
