Black Hole Winds II: Hyper-Eddington Winds and Feedback
  We show that black holes supplied with mass at hyper--Eddington rates drive
outflows with mildly sub--relativistic velocities. These are $\sim 0.1 - 0.2c$
for Eddington accretion factors $\dot m_{\rm acc} \sim 10 - 100$, and $\sim
1500\,{\rm km\, s^{-1}}$ for $\dot m_{\rm acc} \sim 10^4$. Winds like this are
seen in the X--ray spectra of ultraluminous sources (ULXs), strongly supporting
the view that ULXs are stellar--mass compact binaries in hyper--Eddington
accretion states. SS433 appears to be an extreme ULX system ($\dot m_{\rm acc}
\sim 10^4$) viewed from outside the main X--ray emission cone. For less extreme
Eddington factors $\dot m_{\rm acc} \sim 10 - 100$ the photospheric
temperatures of the winds are $\sim 100$\, eV, consistent with the picture that
the ultraluminous supersoft sources (ULSs) are ULXs seen outside the
medium--energy X--ray beam, unifying the ULX/ULS populations and SS433
(actually a ULS but with photospheric emission too soft to detect). For
supermassive black holes (SMBHs), feedback from hyper--Eddington accretion is
significantly more powerful than the usual near--Eddington (`UFO') case, and if
realised in nature would imply $M - \sigma$ masses noticeably smaller than
observed. We suggest that the likely warping of the accretion disc in such
cases may lead to much of the disc mass being expelled, severely reducing the
incidence of such strong feedback. We show that hyper--Eddington feedback from
bright ULXs can have major effects on their host galaxies. This is likely to
have important consequences for the formation and survival of small galaxies.
