Massive gaseous discs around SMBH binaries: Binary decay and tidal disruptions
1 Departamento de Astronomía y Astrofísica, Pontificia Universidad Católica de Chile, Chile
2 Max-Planck-Institut für Gravitationsphysik (Albert Einstein Institute), Am Mühlenberg 1, 14476 Potsdam, Germany
a e-mail: firstname.lastname@example.org
We investigate the evolution of black hole binaries embedded within geometrically thin gas discs. Our results imply that such discs can produce black hole mergers for relatively low-mass binaries, and that a significant population of eccentric binaries might exist at separations of a few 0.01 pc. These binaries may be detectable due to the time-variable accretion on to the black holes. If the disc fragments, then the newly-born stars will continue driving the binary to its coalescence, although at a slower rate. Interestingly, our preliminary analysis shows that these stars will be disrupted at a rate of ∼10−4–2 · 10−5 events per year per system.
© Owned by the authors, published by EDP Sciences, 2012
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