  We present a self-consistent, bimodal stationary solution for spherically
symmetric flows driven by young massive stellar clusters with a central
supermassive black hole. We demonstrate that the hydrodynamic regime of the
flow depends on the location of the cluster in the 3D (star cluster mechanical
luminosity - BH mass - star cluster radius) parameter space. We show that a
threshold mechanical luminosity (L_crit) separates clusters which evolve in the
BH dominated regime frome those whose internal structure is strongly affected
by the radiative cooling. In the first case(below the threshold energy) gravity
of the BH separates the flow into two distinct zones: the inner accretion zone
and the outer zone where the star cluster wind is formed. In the second case
(above the critical luminosity), catastrophic cooling sets in inside the
cluster. In this case the injected plasma becomes thermally unstable that
inhibits a complete stationary solution. We compared the calculated accretion
rates and the BH luminosities with those predicted by the classic Bondi
accretion theory and found that Bondi's theory is in good agreement with our
results in the case of low mass clusters. However, it substantially
underestimates the accretion rates and BH luminosities if the star cluster
mechanical luminosity, L_sc, approaches the threshold value (L_sc > 0.1
L_crit).
