Schematic geometry of the accretion flow in IGR J17091. The accretion disk dominated by radiation pressure (thin solid line) is stabilized by a quasi-static corona in its inner parts and by the unbound wind ejected at its outer radii (its velocity field is marked by arrows). The wind (we show only the first component, for clarity) is partially collimated, and its radial extension in the observed wind is somewhat narrower than at its base.