Formation of discs around super-massive black hole binaries

Abstract

We model numerically the evolution of $10^4{M}_{\odot }$ turbulent molecular clouds in near-radial infall onto $10^6{M}_{\odot }$, 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.

4 pages, 4 figures, Proceedings IAU Symposium No. 312, 2014. Animations available at http://www.astro.puc.cl/~fgarrido/animations

References in corpus (7)

• SPLASH: An interactive visualisation tool for Smoothed Particle Hydrodynamics simulations
• Massive black hole binary mergers within sub-pc scale gas discs
• Tearing up the disc: misaligned accretion on to a binary
• Star Formation Around Super-Massive Black Holes
• Massive binary black holes in galactic nuclei and their path to coalescence
• Migration of massive black hole binaries in self--gravitating accretion discs: Retrograde versus prograde
• Misaligned accretion on to supermassive black hole binaries