Hard X-rays from the BH hot inner corona scattered on Polish donut funnel walls. The funnel model and thick accretion disk are from analytical (left) and numerical simulations (right) (the values of the envelope are digitized from Figure 1 of Q. Lei et al. 2009 in units of gravitational radii). Scattering of hard X-rays is depicted for the proxy model of Cygnus X-3 (A. Veledina et al. 2024).