  The mounting evidence for violent nuclear star formation in Seyfert galaxies
has led us to consider the hydrodynamics of the matter reinserted by massive
stars through strong stellar winds and supernovae, under the presence of a
central massive BH. We show that in all cases there is a bimodal solution
strongly weighted by the location of the stagnation radius (Rst), which splits
the star cluster into two different zones. Matter reinserted within the
stagnation volume is to be accreted by the BH while its outer counterpart would
composed a star cluster wind. The mechanical power of the latter, ensures that
there is no accretion of the ISM into the BH and thus the BH accretion and its
luminosity is regulated by the star formation feedback. The location of the
stagnation radius is a function of three parameters: the BH mass, the
mechanical power (or mass) of the star formation event and the size of the star
forming region. Here we present our self-consistent, stationary solution,
discuss the accretion rates and BH luminosities and show that our model
predicts the intrinsic link between the BH activity and the starburst
parameters.
