  We present results from an investigation of the dynamical behavior of buoyant
magnetic flux rings in the radiative interior of a uniformly rotating
early-type star. Our physical model describes a thin, axisymmetric, toroidal
flux tube that is released from the outer boundary of the convective core, and
is acted upon by buoyant, centrifugal, Coriolis, magnetic tension, and
aerodynamic drag forces. We find that rings emitted in the equatorial plane can
attain a stationary equilibrium state that is stable with respect to small
displacements in radius, but is unstable when perturbed in the meridional
direction. Rings emitted at other latitudes travel toward the surface along
trajectories that largely parallel the rotation axis of the star. Over much of
the ascent, the instantaneous rise speed is determined by the rate of heating
by the absorption of radiation that diffuses into the tube from the external
medium. Since the time scale for this heating varies like the square of the
tube cross-sectional radius, for the same field strength, thin rings rise more
rapidly than do thick rings. For a reasonable range of assumed ring sizes and
field strengths, our results suggest that buoyancy is a viable mechanism for
bringing magnetic flux from the core to the surface, being capable of
accomplishing this transport in a time that is generally much less than the
stellar main sequence lifetime.
