  In this paper we present the first set of 3D magnetohydrodynamic (MHD)
simulations performed with the riemann geomesh code. We study the dynamics of
the magnetically channeled winds of magnetic massive stars in full three
dimensions using a code that is uniquely suited to spherical problems.
Specifically, we perform isothermal simulations of a smooth wind on a rotating
star with a tilted, initially dipolar field. We compare the mass-loss, angular
momentum loss, and magnetospheric dynamics of a template star (with the
properties that are reminiscent of the O4 supergiant {\zeta} Pup) over a range
of rotation rates, magnetic field strengths, and magnetic tilt angles. The
simulations are run up to a quasi-steady state and the results are observed to
be consistent with the existing literature, showing the episodic centrifugal
breakout events of the mass outflow, confined by the magnetic field loops that
form the closed magnetosphere of the star. The catalogued results provide
perspective on how angular-momentum loss varies for different configurations of
rotation rate, magnetic field strength, and large magnetic tilt angles. In
agreement with previous 2D MHD studies, we find that high magnetic confinement
reduces the overall mass-loss rate, and higher rotation increases the mass-loss
rate. This and future studies will be used to estimate the angular-momentum
evolution, spin-down time, and mass-loss evolution of magnetic massive stars as
a function of magnetic field strength, rotation rate, and dipole tilt.
