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The hierarchical galaxy formation picture suggests that super massive blackholes (MBHs) observed in galactic nuclei today have grown from coalescence ofmassive black hole binaries (MBHB) after galaxy merging. Once the components ofa MBHB become gravitationally bound, strong three-body encounters between theMBHB and stars dominate its evolution in a "dry" gas free environment, andchange the MBHB's energy and angular momentum (semi-major axis, eccentricityand orientation). Here we present high accuracy direct N-body simulations ofspherical and axisymmetric (rotating) galactic nuclei with order a millionstars and two massive black holes that are initially unbound. We analyze theproperties of the ejected stars due to slingshot effects from three-bodyencounters with the MBHB in detail. Previous studies have investigated theeccentricity and energy changes of MBHs using approximate models or Monte-Carlothree body scatterings. We find general agreement with the average results ofprevious semi-analytic models for spherical galactic nuclei, but our resultsshow a large statistical variation. Our new results show many more phase spacedetails of how the process works, and also show the influence of stellar systemrotation on the process. We detect that the angle between the orbital plane ofthe MBHBs and that of the stellar system (when it rotates) influences thephase-space properties of the ejected stars. We also find that massive MBHBtend to switch stars with counter-rotating orbits into co-rotating orbitsduring their interactions.

The Link Between Ejected Stars, Hardening and Eccentricity Growth of Super Massive Black Holes in Galactic Nuclei