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

Magnetically Ejected Disks: Equatorial Outflows Near Vertically Magnetized Black Hole