  In this paper we report the results of axisymmetric relativistic MHD
simulations for the problem of Kerr black hole immersed into a rarefied plasma
with ''uniform'' magnetic field. The long term solution shows properties which
are significantly different from those of the initial transient phase studied
recently by Koide(2003). The topology of magnetic field lines within the
ergosphere is similar to that of the split-monopole model with a strong current
sheet in the equatorial plane. Closer inspection reveals a system of isolated
magnetic islands inside the sheet and ongoing magnetic reconnection. No regions
of negative hydrodynamic ''energy at infinity'' are seen inside the ergosphere
and the so-called MHD Penrose process does not operate. Yet, the rotational
energy of the black hole continues to be extracted via purely electromagnetic
mechanism of Blandford and Znajek(1977). However, this is not followed by
development of strong relativistic outflows from the black hole. Combined with
results of other recent simulations this signals a potential problem for the
standard MHD model of relativistic astrophysical jets should they still be
observed at distances as small as few tens of gravitational radii from the
central black hole.
