  The brightest steady sources of radiation in the universe, active galactic
nuclei (AGN), are powered by gas accretion onto a central supermassive black
hole (SMBH). The large sizes and accretion rates implicated in AGN accretion
disks are expected to lead to gravitational instability and fragmentation,
effectively cutting off mass inflow to the SMBH. Radiative feedback from
disk-embedded stars has been invoked to yield marginally stable, steady-state
solutions in the outer disks. Here, we examine the consequences of this star
formation with a semi-analytical model in which stellar-mass black hole (sBH)
remnants in the disk provide an additional source of stabilizing radiative
feedback. Assuming star formation seeds the embedded sBH population, we model
the time-evolving feedback from both stars and the growing population of
accreting sBHs. We find that in the outer disk, the luminosity of the sBHs
quickly dominates that of their parent stars. However, because sBHs consume
less gas than stars to stabilize the disk, the presence of the sBHs enhances
the mass flux to the inner disk. As a result, star formation persists over the
lifetime of the AGN, damped in the outer disk, but amplified in a narrow ring
in the inner disk. Heating from the embedded sBHs significantly modifies the
disk's temperature profile and hardens its spectral energy distribution, and
direct emission from the sBHs adds a new hard X ray component, resembling a
Compton reflection "hump".
