radius, the centrifugal forces will become important before the gas reaches the horizon. In this case, the gas will be thrown into near circular orbits and only after viscous stresses have transported away the excess of angular momentum will the gas cross the BH horizon (Shvartsman 1971). In fact, the formation or not of a disk requires two conditions: the disk radius must be larger than the last stable circular orbit (equivalent to the condition $J > 2r_gc$) and must be smaller than the typical dimension of the shock cone, e.g., $l_s \approx 2r_g(c/u_{\infty})^2$, where $u_{\infty}$ is the BH velocity with respect to the gas. If the gas is highly turbulent, the velocity of eddies having a scale $k$ is given roughly by $$V_t \sim V_0\left(\frac{k}{k_0}\right)^q$$ In the case of a Kolmogorov spectrum, $q = 1/3$. However, it is more probable that the turbulent energy be dissipated mainly through shock waves and, in this case, the spectrum is steeper with $q \sim 1$ (Kaplan 1954), a situation which will be assumed here. For our rough estimates, we adopt typical values for the turbulence observed in our Galaxy, e.g., $V_0 \approx 10~ km.s^{-1}$, $k_0 \approx 10~ pc$ (Kaplan & Pikel’ner 1970). 