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Simulating the dynamics of binary black holes in nuclear gaseous discs

Published online by Cambridge University Press:  01 July 2007

Massimo Dotti
Affiliation:
Dipartimento di Fisica e Matematica, Università dell'Insubria, 22100, Como, Italy email: dotti@mib.infn.it
Monica Colpi
Affiliation:
Dipertimento di Fisica G. Occhialini, Università di Milano Bicocca, 20126 Milano, Italy
Francesco Haardt
Affiliation:
Dipartimento di Fisica e Matematica, Università dell'Insubria, 22100, Como, Italy email: dotti@mib.infn.it
Lucio Mayer
Affiliation:
Institute for Theoretical Physics, University of Zurich, CH-8057, Zurich, Switzerland Institute of Astronomy, Department of Physics, ETH, Zurich, HC-8095 Zurich, Switzerland
Corresponding
E-mail address:
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Abstract

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Dotti, M., Colpi, M., & Haardt, F. 2006, MNRAS 367, 103CrossRefGoogle Scholar
Dotti, M., Colpi, M., Haardt, F., & Mayer, L. 2007, MNRAS 379, 956CrossRefGoogle Scholar
Escala, A., Larson, R. B., Coppi, P. S., & Maradones, D. 2005, ApJ 630, 152CrossRefGoogle Scholar
Kitsionas, S. & Whitworth, S. 2002, MNRAS 330, 129CrossRefGoogle Scholar
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