2026ApJ..1000...77L

It is widely believed that stellar-mass black holes (sMBHs) exist within the accretion disks of active galactic nuclei (AGN), forming a distinct population termed “accretion-modified star” (AMS). Gas from the dense disk accretes onto these AMSs, dissipating substantial gravitational energy through a minidisk around the sMBHs, which drives powerful outflows that interact with the surrounding disk gas. In this study, we investigate two scenarios for AMS accretion: episodic Bondi explosions with hyper-Eddington accretion (Scenario A) and steady Eddington accretion (Scenario B). These outflows generate turbulence, facilitating outward angular momentum transport in the AGN disk via shock interactions and angular momentum exchange. We explore a broad parameter space, spanning the central supermassive black hole (SMBH) mass (M_p), dimensionless accretion rate (${\dot{{\mathscr{M}}}}_{{\rm{p}}}$), sMBH mass function, and spatial distribution to calculate the effective viscosity parameter α_AMS. Our analysis reveals the scaling relations ${\alpha }_{{\rm{AMS}}}\propto \zeta {M}_{{\rm{p}}}^{2}{\dot{{\mathscr{M}}}}_{{\rm{p}}}$ for Scenario A and ${\alpha }_{{\rm{AMS}}}\propto \zeta {M}_{{\rm{p}}}^{1.5}{\dot{{\mathscr{M}}}}_{{\rm{p}}}^{0.1}$ for Scenario B, where ζ denotes the ratio of the total sMBH mass to the SMBH disk mass. For ζ = 0.01 and M_p = 10⁸M_⊙, α_AMS ranges from ∼3 × 10^–4 to 0.01 (Scenario A) and ∼3 × 10^–3 to 0.04 (Scenario B) from the inner to outer disk regions. These results demonstrate that AMS feedback provides an efficient mechanism for angular momentum transport in AGN disks.