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

Abstract

We present 1D numerical simulations, which consider the effects of radiative cooling and gravity on the hydrodynamics of the matter reinserted by stellar winds and supernovae within young nuclear starbursts with a central supermassive black hole (SMBH). The simulations confirm our previous semi-analytic results for low energetic starbursts, evolving in a quasi-adiabatic regime, and extend them to more powerful starbursts evolving in the catastrophic cooling regime. The simulations show a bimodal hydrodynamic solution in all cases. They present a quasi-stationary accretion flow onto the black hole, defined by the matter reinserted by massive stars within the stagnation volume and a stationary starburst wind, driven by the high thermal pressure acquired in the region between the stagnation and the starburst radii. In the catastrophic cooling regime, the stagnation radius rapidly approaches the surface of the starburst region, as one considers more massive starbursts. This leads to larger accretion rates onto the SMBH and concurrently to powerful winds able to inhibit interstellar matter from approaching the nuclear starburst. Our self-consistent model thus establishes a direct physical link between the SMBH accretion rate and the nuclear star formation activity of the host galaxy and provides a good upper limit to the accretion rate onto the central black hole.

20 pages, 6 figures, accepted for publication in The Astrophysical Journal.

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Cited by in corpus (8)

• An expanded M_bh-sigma diagram, and a new calibration of active galactic nuclei masses
• Extending the M_(bh)-sigma diagram with dense nuclear star clusters
• The formation of secondary stellar generations in massive young star clusters from rapidly cooling shocked stellar winds
• On the Onset of Secondary Stellar Generations in Giant Star Forming Regions and Massive Star Clusters
• The Role of Nuclear Star Clusters in Enhancing Supermassive Black Hole Feeding Rates During Galaxy Mergers
• Should I Stay or Should I Go: Stellar Wind Retention and Expulsion in Massive Star Clusters
• Modeling Gas Evacuation Mechanisms in Present-Day Globular Clusters: Stellar Winds from Evolved Stars and Pulsar Heating
• On the fate of the matter reinserted within young nuclear stellar clusters