Can Stellar-mass Black Hole Growth Disrupt Disks of Active Galactic Nuclei? The Role of Mechanical Feedback

Stellar-mass BHs (sBHs) are predicted to be embedded in active galactic nuclei (AGN) disks due gravitational drag and in-situ star formation. However, we find that a high gas density an AGN disk environment, compact objects may rapidly grow intermediate-mass deplete matter from the unless accretion is suppressed by some feedback process(es). These consequences inconsistent with observations dynamics of Galactic center. Here consider mechanical mechanisms for reduction accretion. Rapidly accreting sBHs launch winds and/or jets via Blandford-Znajek mechanism, which produce high-pressure shocks cocoons. Such shock cocoon can spread laterally plane disk, eject outer regions circum-sBH (CsBD) puncture hole horizontal size comparable scale-height. Since depletion timescale bound CsBD much shorter than resupply sBH, time-averaged rate onto reduced this process factor $\sim 10$--$100$. This mechanism therefore help alleviate sBH over-growth AGN-disk problems. On other hand, cocoons unbind large fraction less massive SMBHs, explain dearth high-Eddington ratio AGNs SMBH mass $\lesssim10^5{\rm M_\odot}$.