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• W1939384555 startingPage "1591" @default.
• W1939384555 abstract "We investigate whether a circumbinary gas disc can coalesce a supermassive black hole binary system in the centre of a galaxy. This is known to be problematic for a prograde disc. We show that in contrast, interaction with a retrograde circumbinary disc is considerably more effective in shrinking the binary because there are no orbital resonances. The binary directly absorbs negative angular momentum from the circumbinary disc by capturing gas into a disc around the secondary black hole, or discs around both holes if the binary mass ratio is close to unity. In many cases the binary orbit becomes eccentric, shortening the pericentre distance as the eccentricity grows. In all cases the binary coalesces once it has absorbed the angular momentum of a gas mass comparable to that of the secondary black hole. Importantly, this conclusion is unaffected even if the gas inflow rate through the disc is formally super--Eddington for either hole. The coalescence timescale is therefore always $sim M_2/dot M$, where $M_2$ is the secondary black hole mass and $dot M$ the inflow rate through the circumbinary disc." @default.
• W1939384555 created "2016-06-24" @default.
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• W1939384555 date "2011-03-17" @default.
• W1939384555 modified "2023-10-14" @default.
• W1939384555 title "Retrograde accretion and merging supermassive black holes" @default.
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• W1939384555 doi "https://doi.org/10.1111/j.1365-2966.2010.17952.x" @default.
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