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Formation of discs around super-massive black hole binaries

Published online by Cambridge University Press:  07 March 2016

Felipe G. Goicovic ,
Jorge Cuadra  and
Alberto Sesana
Felipe G. Goicovic
Affiliation:
Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile email: fgarrido@astro.puc.cl
Jorge Cuadra
Affiliation:
Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Santiago, Chile email: fgarrido@astro.puc.cl
Alberto Sesana
Affiliation:
Max-Planck-Institut für Gravitationsphysik, Potsdam-Golm, Germany
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Abstract

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We model numerically the evolution of 104M⊙ turbulent molecular clouds in near-radial infall onto 106M⊙, equal-mass supermassive 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.

Keywords

black hole physicsaccretion discshydrodynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S312: Star Clusters and Black Holes in Galaxies across Cosmic Time , August 2014 , pp. 48 - 51
Copyright
Copyright © International Astronomical Union 2016 

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