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Using numerical simulations we present the accretion of supersonic winds ontoa rotating black hole in three dimensions. We study five representativedirections of the wind with respect to the axis of rotation of the black holeand focus on the evolution and stability of the high density shock cone that isformed during the process. We explore both, the regime in which the shock coneis expected to be stable in order to confirm previous results obtained with twodimensional simulations, and the regime in which the shock cone is expected toshow a flip-flop type of instability. The methods used to attempt triggeringthe instability were first the accumulation of numerical errors and second theexplicit application of a perturbation on the velocity field after theshock-cone was formed. The result is negative, that is, we did not find theflip-flop instability within the parameter space we explored, which includescases that are expected to be unstable.

Accretion of supersonic winds onto black holes in 3D: stability of the shock cone