  We summarize recent 2D MHD simulations of line-driven stellar winds from
rotating hot-stars with a dipole magnetic field aligned to the star's rotation
axis. For moderate to strong fields, much wind outflow is initially along
closed magnetic loops that nearly corotate as a solid body with the underlying
star, thus providing a torque that results in an effective angular momentum
spin-up of the outflowing material. But instead of forming the ``magnetically
torqued disk'' (MTD) postulated in previous phenemenological analyses, the
dynamical simulations here show that material trapped near the tops of such
closed loops tends either to fall back or break out, depending on whether it is
below or above the Keplerian corotation radius. Overall the results raise
serious questions about whether magnetic torquing of a wind outflow could
naturally result in a Keplerian circumstellar disk. However, for very strong
fields, it does still seem possible to form a %``magnetically confined,
centrifugally supported, rigid-body disk'', centrifugally supported,
``magnetically rigid disk'' (MRD), in which the field not only forces material
to maintain a rigid-body rotation, but for some extended period also holds it
down against the outward centrifugal force at the loop tops. We argue that such
rigid-body disks seem ill-suited to explain the disk emission from Be stars,
but could provide a quite attractive paradigm for circumstellar emission from
the magnetically strong Bp and Ap stars.
