2012
DOI: 10.1051/0004-6361/201219986
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Evolution of binary black holes in self gravitating discs

Abstract: Context. Massive black hole binaries, formed in galaxy mergers, are expected to evolve in dense circumbinary discs. Understanding of the disc-binary coupled dynamics is vital to assess both the final fate of the system and its potentially observable features. Aims. Aimed at understanding the physical roots of the secular evolution of the binary, we study the interplay between gas accretion and gravity torques in changing the binary elements (semi-major axis and eccentricity) and its total angular momentum budg… Show more

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Cited by 171 publications
(226 citation statements)
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References 63 publications
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“…The two runs discussed below differ only in their BH mass ratio (q = 0.1 and q = 0.5). A wider range of simulations is needed in the future, to address possibilities such as eccentric (Roedig et al 2012), tilted (Hayasaki et al 2015), or retrograde (Nixon et al 2011) binary orbits.…”
Section: Implications Of a Shorter Orbital Periodmentioning
confidence: 99%
See 1 more Smart Citation
“…The two runs discussed below differ only in their BH mass ratio (q = 0.1 and q = 0.5). A wider range of simulations is needed in the future, to address possibilities such as eccentric (Roedig et al 2012), tilted (Hayasaki et al 2015), or retrograde (Nixon et al 2011) binary orbits.…”
Section: Implications Of a Shorter Orbital Periodmentioning
confidence: 99%
“…Binaries with 0.3 ∼ < q ∼ < 0.8 clear a lopsided central cavity in the disc, causing variability on three time-scales. The dominant period, (3 − 8)t bin is that of an over dense lump, orbiting at the ridge of the cavity, with additional periodicities at t bin and ≈ 0.5t bin (MacFadyen & Milosavljević 2008;Shi et al 2012;Noble et al 2012;Roedig et al 2012;D'Orazio et al 2013;Farris et al 2014). The dominant period depends on the size of the cavity, and thus on disc parameters, such as temperature and viscosity.…”
Section: Introductionmentioning
confidence: 99%
“…More specifically, if the binary is embedded in a thin disk, the gas will be expelled from the central region due to torques exerted by the binary, creating a cavity (Artymowicz & Lubow 1994). Several hydrodynamical simulations (Hayasaki, Mineshige & Sudou 2007;MacFadyen & Milosavljević 2008;Noble et al 2012;Shi et al 2012;Roedig et al 2012;D'Orazio, Haiman & MacFadyen 2013;Farris et al 2014) indicate that the interaction of the individual BHs with the inner edge of the accretion disk can pull gaseous streams into the cavity, resulting in periodic modulation of the accretion rate at timescales corresponding to ≈1/2 and 1 times the binary's orbital period. For high BH mass ratios (q ≡ M1/M2 ∼ > 0.3), the cavity is lopsided, leading to the formation of a hotspot in the accretion disk.…”
Section: Introductionmentioning
confidence: 99%
“…(MacFadyen and Milosavljević 2008;Roedig et al 2012;Shi et al 2012). The above expression for the torque relates the rate of binary orbital decay to the local disc mass M edge d…”
Section: Mestel Imentioning
confidence: 99%