Simulating the dynamics of binary black holes in nuclear gaseous discs

Details Simulating the dynamics of binary black holes in nuclear gaseous discs Simulating the dynamics of binary black holes in nuclear gaseous discs

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..245..241d&link_type=abstract

Formation and Evolution of Galaxy Bulges, Proceedings of the International Astronomical Union, IAU Symposium, Volume 245, p. 241

Physics

Black Hole Physics, Hydrodynamics, Galaxies: Evolution, Galaxies: Nuclei, Galaxies: Starburst

Scientific paper

We study the pairing of massive black holes embedded in a massive circum nuclear, rotationally supported disc, until they form a close binary. Using high resolution SPH simulations, we follow the black hole dynamics, and in particular the eccentricity evolution, as a function of the composition in stars and gas of the disc. Binary disc interaction always leads to orbital decay and, in case of co rotating black holes, to orbit circularization. We present also a higher resolution simulation performed using the particle splitting technique showing that the binary orbital decay is efficient down to a separation of ~ 0.1 pc, comparable to our new resolution limit. We detail the gaseous mass profile bound to each black hole. Double nuclear activity is expected to occur on an estimated timescale of ≲ 10 Myrs.

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