  Accreting black hole sources show variable outflows at different mass scales.
For instance, in the case of galactic nuclei, our own galactic center Sgr A*
exhibits flares and outbursts in the X-ray and infrared bands. Recent studies
suggest that the inner magnetospheres of these sources have a pronounced effect
on such emissions. Accreting plasma carries the frozen-in magnetic flux along
with it down to the black hole horizon. During the in-fall, the magnetic field
intensifies and it can lead to a magnetically arrested state. We investigate
the competing effects of inflows at the black hole horizon and the outflows
developed in the accreting plasma due to the action of magnetic field in the
inner magnetosphere and their implications. We start with a spherically
symmetric Bondi-type inflow and introduce the magnetic field. In order to
understand the influence of the initial configuration, we start the
computations with an aligned magnetic field with respect to the black hole
rotation axis. Then we proceed to the case of magnetic fields inclined to the
black hole rotation axis. We employ the 2D and 3D versions of HARM code for the
aligned field models while using the 3D version for the inclined field and
compare the results of computations against each other. We observe how the
magnetic lines of force start accreting with the plasma while an equatorial
intermittent outflow develops and goes on pushing some material away from the
black hole partially along the equatorial plane, and partly ejecting it out of
the plane in the vertical direction. In consequence, the accretion rate also
fluctuates. The black hole spin direction prevails at later stages and it
determines the flow geometry near the event horizon, whereas on larger scales
the flow geometry stays influenced by the initial inclination of the field.
