How the super-Eddington regime regulates black hole growth in
  high-redshift galaxies
  Super-Eddington accretion is one scenario that may explain the rapid assembly
of $\sim 10^9\rm\, M_\odot$ supermassive black holes (BHs) within the first
billion year of the Universe. This critical regime is associated with
radiatively inefficient accretion and accompanied by powerful outflows in the
form of winds and jets. By means of hydrodynamical simulations of BH evolution
in an isolated galaxy and its host halo with 12 pc resolution, we investigate
how super-Eddington feedback affects the mass growth of the BH. It is shown
that super-Eddington feedback efficiently prevents BH growth within a few Myr.
The super-Eddington accretion events remain relatively mild with typical rates
of about 2-3 times the Eddington limit, because of the efficient regulation by
jets in that regime. We find that these jets are powerful enough to eject gas
from the centre of the host galaxy all the way up to galactic scales at a few
kpc, but do not significantly impact gas inflows at those large scales. By
varying the jet feedback efficiency, we find that weaker super-Eddington jets
allow for more significant BH growth through more frequent episodes of
super-Eddington accretion. We conclude that effective super-Eddington growth is
possible, as we find that simulations with weak jet feedback efficiencies
provide a slightly larger BH mass evolution over long periods of time ($\sim
80\,\rm Myr$) than that for a BH accreting at the Eddington limit.
