Mergers of Black Holes in the Galactic Center

Abstract

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 P11 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.

Intermediate-mass black holes as LISA sources

“…More recently, Koch and Hansen [15] explored additional effects, such as the interactions of IMBHs with themselves around an SMBH, assuming that the full coalescence process takes longer than the time needed for new clusters and IMBHs to sink to the center. They found that such encounters tend to eject one IMBH (although slowly, so that it will sink back in), and leave the other in an eccentric orbit that decays readily by emission of gravitational radiation.…”