  Strong gravity and magnetic fields are key ingredients that power processes
of accretion and ejection near compact objects. While the particular mechanisms
that operate here are still discussed, it seems that the presence of an ordered
magnetic field is crucial for the acceleration and collimation of relativistic
jets of electrically charged particles on superhorizon length scales. In this
context, we further study the effect of a large-scale magnetic field on the
dynamics of charged particles near a rotating black hole. We consider a
scenario in which the initially neutral particles on regular geodesic orbits in
the equatorial plane are destabilized by a charging process (e.g., by
photoionization). Some charged particles are accelerated out of the equatorial
plane, and they follow jetlike trajectories with relativistic velocities. In
our previous paper, we investigated this scenario for the case of perfect
alignment of the magnetic field with the axis of rotation; i.e., the system was
considered axisymmetric. Here we relax this assumption and investigate
nonaxisymmetric systems in which the magnetic field is arbitrarily inclined
with respect to the black hole spin. We study the system numerically in order
to locate the zones of escaping trajectories and compute the maximum (terminal)
escape velocity. It appears that breaking the axial symmetry (even by small
inclination angles) substantially increases the fraction of escaping orbits and
allows the acceleration to ultrarelativistic velocities that were excluded in
the axisymmetric setup. The presence of transient chaotic dynamics in the
launching region of the relativistic outflow is confirmed with chaotic
indicators.
