  We present 3D general relativistic magnetohydrodynamic(GRMHD) simulations of
zero angular momentum accretion around a rapidly rotating black hole, modified
by the presence of initially uniform magnetic fields. We consider serveral
angles between the magnetic field direction and the black hole spin. In the
resulting flows, the midplane dynamics are governed by magnetic
reconnection-driven turbulence in a magnetically arrested (or a nearly
arrested) state. Electromagnetic jets with outflow efficiencies ~10-200% occupy
the polar regions, reaching several hundred gravitational radii before they
dissipate due to the kink instability. The jet directions fluctuate in time and
can be tilted by as much as ~30 degrees with respect to black hole spin, but
this tilt does not depend strongly on the tilt of the initial magnetic field. A
jet forms even when there is no initial net vertical magnetic flux since
turbulent, horizon-scale fluctuations can generate a net vertical field
locally. Peak jet power is obtained for an initial magnetic field tilted by
40-80 degrees with respect to the black hole spin because this maximizes the
amount of magnetic flux that can reach the black hole. These simulations may be
a reasonable model for low luminosity black hole accretion flows such as Sgr A*
or M87.
