  General-relativistic magneto-hydrodynamical (GRMHD) simulations of accreting
black holes suggest that the accretion flows form toroidal structures embedded
in a large scale component of magnetic field, which becomes organized on
length-scales exceeding the gravitational radius of the central black hole.
Magnetic field grows gradually until a Magnetically Arrested Disc (MAD)
develops that diminishes or inhibits further accretion. We study an outflow
that develops in the MAD state in 3D GRMHD simulations. We show that the
outflow can be accelerated to relativistic velocities and persist over the
course of our simulation. We compare the properties of the outflow from MAD
discs with those launched by orbiting secondary at close orbit. The main
difference is that the orbiting body launches a more coherent, quasiperiodic
ultrafast outflow at lower velocities ($v<0.5c$) while the outflow launched in
the MAD state (without the body) has a stochastic behaviour and has an
approximately flat velocity distribution between lower and higher outflow
velocities, $0.2c<v<0.3c$ and $v>0.5c$.
