Abstract
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.
Highlights
Galaxies form via mergers of lower mass progenitors, most of which host supermassive black holes (SMBHs)
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
Summary
Galaxies form via mergers of lower mass progenitors, most of which host supermassive black holes (SMBHs). The SMBHs sink toward the centre of the merger product and form a binary. What happens is less clear: angular momentum loss to either stars or gas is required to bring the black holes into the gravitational radiation inspiral regime, in which the coalescence occurs rapidly. Prior work has established that nuclear gas discs are likely to be important for SMBH binary mergers (Armitage & Natarajan 2002; Escala et al 2005; Dotti et al 2007; MacFadyen & Milosavljevic 2008). We revisit the interaction between a SMBH binary and a relatively low mass circumbinary gas disc. For further details refer to our full-length papers (Cuadra et al 2009; Roedig et al 2011; Amaro-Seoane, Brem & Cuadra, in prep.)
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