  We present results from new self-consistent 3D MHD simulations of the
magnetospheres from massive stars with a dipole magnetic axis that has a
non-zero obliquity angle ($\beta$) to the star's rotation axis. As an initial
direct application, we compare the global structure of co-rotating disks for
nearly aligned ($\beta=5^o$) versus half-oblique ($\beta=45^o$) models, both
with moderately rapid rotation ($\sim$ 0.5 critical). We find that accumulation
surfaces broadly resemble the forms predicted by the analytic Rigidly Rotating
Magnetosphere (RRM) model, but the mass buildup to near the critical level for
centrifugal breakout against magnetic confinement distorts the field from the
imposed initial dipole. This leads to an associated warping of the accumulation
surface toward the rotational equator, with the highest density concentrated in
{\em wings} centered on the intersection between the magnetic and rotational
equators. These MHD models can be used to synthesize rotational modulation of
photometric absorption and H$\alpha$ emission for a direct comparison with
observations.
