  We present the accretion of magnetized supersonic winds onto a rotating black
hole in three dimensions. We select representative spin-wind orientations in
order to illustrate its effects on the evolution and morphology of the shock
cone. The most important finding in the magnetized case, unlike the purely
hydrodynamical scenario, is the formation of rarified spots where the magnetic
field pressure dominates over the gas pressure. In these rarified spots we find
the formation of eddies within the shock cone.
