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Simulating the dynamics of binary black holes in nuclear gaseous discs

Dotti, Massimo ; Colpi, Monica ; Haardt, Francesco ; Mayer, Lucio

In: Proceedings of the International Astronomical Union, 2007, vol. 3, no. S245, p. 241-242

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    Titre
    • Simulating the dynamics of binary black holes in nuclear gaseous discs
    Auteur
    • Dotti, Massimo. Dipartimento di Fisica e Matematica, Università dell'Insubria, 22100, Como, Italy email: dotti@mib.infn.it
    • Colpi, Monica. Dipertimento di Fisica G. Occhialini, Università di Milano Bicocca, 20126 Milano, Italy
    • Haardt, Francesco. Dipartimento di Fisica e Matematica, Università dell'Insubria, 22100, Como, Italy email: dotti@mib.infn.it
    • Mayer, Lucio. Institute for Theoretical Physics, University of Zurich, CH-8057, Zurich, Switzerland
    Type de document
    • Postprint
    Langue
    • Anglais
    Publié dans
    • Proceedings of the International Astronomical Union, 2007, vol. 3, no. S245, p. 241-242. Cambridge University Press
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:295535
    Summary
    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