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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 

References

Amaro-Seoane, P., Brem, P., & Cuadra, J. 2013, ApJ, 764, 14CrossRefGoogle Scholar
Armitage, P. J. & Natarajan, P. 2005, ApJ, 634, 921CrossRefGoogle Scholar
Begelman, M. C., Blandford, R. D., & Rees, M. J. 1980, Nature, 287, 307CrossRefGoogle Scholar
Bonnell, I. A. & Rice, W. K. M. 2008, Science, 321, 1060CrossRefGoogle Scholar
Colpi, M. 2014, SSR, 183, 189Google Scholar
Cuadra, J., Armitage, P. J., Alexander, R. D., & Begelman, M. C. 2009, MNRAS, 393, 1423CrossRefGoogle Scholar
Dunhill, A. C., Alexander, R. D., Nixon, C. J., & King, A. R. 2014, MNRAS, 445, 2285CrossRefGoogle Scholar
Hobbs, A., Nayakshin, S., Power, C., & King, A. 2011, MNRAS, 413, 2633CrossRefGoogle Scholar
Nixon, C., King, A., & Price, D. 2013, MNRAS, 434, 1946CrossRefGoogle Scholar
Price, D. J., 2007, PASA, 24, 159CrossRefGoogle Scholar
Richstone, D., et al. 1998, Nature, 395Google Scholar
Roedig, C. & Sesana, A. 2014, MNRAS, 439, 3476CrossRefGoogle Scholar
Springel, V. 2005, MNRAS, 364, 1105CrossRefGoogle Scholar
Yu, Q. 2002, MNRAS, 331, 935CrossRefGoogle Scholar