  We present first results of a long-term project which aims at multi-scale,
multi-physics simulations of wind accretion in microquasars and high-mass X-ray
binaries. The 3D hydrodynamical simulations cover all scales, from the
circum-binary environment down to the immediate vicinity of the black hole. We
first introduce the numerical method and parallelization strategy of the AMR
A-MAZE code. We then discuss some preliminary results of how, and on what
scales, an accretion disk is formed around the black hole. We finally present
some characteristics of this disk, which is far from Keplerian. We emphasize
that on all scales shocks play a decisive role for the accretion process and
the process of structure formation -- for the formation of the large scale,
nearly coherent structure of the disk, but also for the formation of turbulent
fluctuations.
