  Using numerical simulations we present the accretion of supersonic winds onto
a rotating black hole in three dimensions. We study five representative
directions of the wind with respect to the axis of rotation of the black hole
and focus on the evolution and stability of the high density shock cone that is
formed during the process. We explore both, the regime in which the shock cone
is expected to be stable in order to confirm previous results obtained with two
dimensional simulations, and the regime in which the shock cone is expected to
show a flip-flop type of instability. The methods used to attempt triggering
the instability were first the accumulation of numerical errors and second the
explicit application of a perturbation on the velocity field after the
shock-cone was formed. The result is negative, that is, we did not find the
flip-flop instability within the parameter space we explored, which includes
cases that are expected to be unstable.
