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We present 1D numerical simulations, which consider the effects of radiativecooling and gravity on the hydrodynamics of the matter reinserted by stellarwinds and supernovae within young nuclear starbursts with a centralsupermassive black hole (SMBH). The simulations confirm our previoussemi-analytic results for low energetic starbursts, evolving in aquasi-adiabatic regime, and extend them to more powerful starbursts evolving inthe catastrophic cooling regime. The simulations show a bimodal hydrodynamicsolution in all cases. They present a quasi-stationary accretion flow onto theblack hole, defined by the matter reinserted by massive stars within thestagnation volume and a stationary starburst wind, driven by the high thermalpressure acquired in the region between the stagnation and the starburst radii.In the catastrophic cooling regime, the stagnation radius rapidly approachesthe surface of the starburst region, as one considers more massive starbursts.This leads to larger accretion rates onto the SMBH and concurrently to powerfulwinds able to inhibit interstellar matter from approaching the nuclearstarburst.  Our self-consistent model thus establishes a direct physical link between theSMBH accretion rate and the nuclear star formation activity of the host galaxyand provides a good upper limit to the accretion rate onto the central blackhole.

On the Hydrodynamic Interplay Between a Young Nuclear Starburst and a Central Super Massive Black Hole