  The first stars in the universe, forming at redshifts z>15 in minihalos with
masses of order 10^6 Msun, may leave behind black holes as their remnants.
These objects could conceivably serve as "seeds" for much larger black holes
observed at redshifts z~6. We study the growth of the remnant black holes
through accretion including for the first time the emitted accretion radiation
with adaptive mesh refinement cosmological radiation-hydrodynamical
simulations. The effects of photo-ionization and heating dramatically affect
the accretion flow from large scales, resulting in negligible mass growth of
the black hole. We compare cases with the accretion luminosity included and
neglected to show that the accretion radiation drastically changes the
environment within 100 pc of the black hole, where gas temperatures are
increased by an order of magnitude. The gas densities are reduced and further
star formation in the same minihalo prevented for the two hundred million years
of evolution we followed. These calculations show that even without the
radiative feedback included most seed black holes do not gain mass as
efficiently as has been hoped for in previous theories, implying that black
hole remnants of Pop III stars that formed in minihalos are not likely to be
the origin of miniquasars. Most importantly, however, these calculations
demonstrate that if early stellar mass black holes are indeed accreting close
to the Bondi-Hoyle rate with ten percent efficiency they have a dramatic local
effect in regulating star formation in the first galaxies.
