  Black holes attract gaseous material from the surrounding environment. Cosmic
plasma is largely ionized and magnetized because of electric currents flowing
in the highly conductive environment near black holes; the process of accretion
then carries the magnetic flux onto the event horizon, $r\simeq R_+$. On the
other hand, magnetic pressure acts against accretion. It can not only arrest
the inflow but it can even push the plasma away from the black hole if the
magnetic repulsion prevails. The black hole does not hold the magnetic field by
itself.
  In this contribution we show an example of an equatorial outflow driven by a
large scale magnetic field. We initiate our computations with a spherically
symmetric distribution of gas, which flows onto the domain from a large
distance, $r\gg R_+$. After the flow settles in a steady (Bondi) solution, we
impose an axially symmetric configuration of a uniform (Wald) magnetic field
aligned with the rotation axis of the black hole. Then we evolve the initial
configuration numerically by employing the MHD code that approaches the
force-free limit of a perfectly conducting fluid.
  We observe how the magnetic lines of force start accreting with the plasma
while an equatorial intermittent outflow develops and goes on ejecting some
material away from the black hole.
