2008/09/29 by Florian Koch, F. Elliott Koch, Bradley M. S. Hansen
Physics and Astronomy · #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1086/591781
Official paper to appear in November 2008 issue of ApJ
arxiv created 2008/09/29 · openalex publication_date 2008/10/24 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We present the results of three-body simulations focused on understanding the fates of intermediate-mass black holes (IBHs) that drift within the central 0.5 pc of the Galaxy. In particular, we modeled the interactions between pairs of 4000 M ☉ black holes as they orbit a central black hole (CBH) of mass 4 × 10 6 M ☉ . The simulations performed assume a Schwarzschild geometry and account for Chandrasekhar dynamical friction as well as acceleration resulting from energy lost due to gravitational radiation. We found the branching ratio for one of the orbiting IBHs to merge with the CBH was 0.95 and is independent of the inner IBH's initial eccentricity as well as the rate of sinking. This, coupled with an infall rate of ~10 7 yr for an IBH to drift into the Galactic center, results in an IBH-CBH merger every ≲11 Myr. Lastly, we found that the IBH-IBH-CBH triple-body system "resets" itself, in the sense that a system with an inner IBH with an initially circular orbit generally left behind an IBH with a large eccentricity, whereas a system in which the inner IBH had a high eccentricity ( e 0 ∼ 0.9) usually left a remnant with low eccentricity. Branching ratios for different outcomes are also similar in the two cases.