  Astrophysical plasmas are often subject to both rotation and large-scale
background magnetic fields. Individually, each is known to two-dimensionalize
the flow in the perpendicular plane. In realistic flows, both of these effects
are simultaneously present and, importantly, need not be aligned. In this work,
we numerically investigate three-dimensional forced magnetohydrodynamic (MHD)
turbulence subject to the competing effects of global rotation and a
perpendicular background magnetic field. We focus on the case of a strong
background field and find that increasing the rotation rate from zero produces
significant changes in the structure of the turbulent flow. Starting with a
two-dimensional inverse cascade at zero rotation, the flow first transitions to
a forward cascade of kinetic energy, then to a shear-layer dominated regime,
and finally to a second shear-layer regime where the kinetic energy flux is
strongly suppressed and the energy transfer is mediated by the induced magnetic
field. We show that the first two transitions occur at distinct values of the
Rossby number, and the third occurs at a distinct value of the Lehnert number.
More generally, our results demonstrate that, when considering the simultaneous
limits of strong rotation and a strong guide field, the order in which those
limits are taken matters in the misaligned case.
