Formation of discs around super-massive black hole binaries
  We model numerically the evolution of $10^4M_\odot$ turbulent molecular
clouds in near-radial infall onto $10^6M_\odot$, equal-mass super-massive black
hole binaries, using a modified version of the SPH code GADGET-3. We
investigate the different gas structures formed depending on the relative
inclination between the binary and the cloud orbits. Our first results indicate
that an aligned orbit produces mini-discs around each black hole, almost
aligned with the binary; a perpendicular orbit produces misaligned mini-discs;
and a counter-aligned orbit produces a circumbinary, counter-rotating ring.
