  This paper presents a survey of a set of simulations of accretion disks
orbiting a rapidly rotating Kerr black hole and embedded in a large-scale
initial magnetic field. Each simulation uses a common state for the initial
torus, including an MRI seed-field consisting of poloidal loops along
isodensity contours, and differ only in the strength of the initial large-scale
magnetic field in relation to these poloidal loops. Simulations with a weak
large-scale initial field differ little from simulations that evolve from only
the poloidal field. Simulations where the large-scale initial field distorts or
completely overwhelms the poloidal loops show more extensive regions of
turbulence, due to the action of the MRI on the large-scale field. However, the
overall structure of the late-time state of the simulations remains
qualitatively unchanged, that is each simulation sees the emergence of a
turbulent accretion disk, axial jets, a funnel-wall outflow and an extensive
corona.
