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In this paper we consider a scenario where the currently observedhypervelocity stars in our Galaxy have been ejected from the Galactic center asa result of dynamical interactions with an intermediate-mass black hole (IMBH)orbiting the central supermassive black hole (SMBH). By performing 3-bodyscattering experiments, we calculate the distribution of the ejected stars'velocities given various parameters of the IMBH-SMBH binary: IMBH mass,semimajor axis and eccentricity. We also calculate the rates of change of theBH binary orbital elements due to those stellar ejections. One of our newfindings is that the ejection rate depends (although mildly) on the rotation ofthe stellar nucleus (its total angular momentum). We also compare the ejectionvelocity distribution with that produced by the Hills mechanism (stellar binarydisruption) and find that the latter produces faster stars on average. Also,the IMBH mechanism produces an ejection velocity distribution which isflattened towards the BH binary plane while the Hills mechanism produces aspherically symmetric one. The results of this paper will allow us in thefuture to model the ejection of stars by an evolving BH binary and compare bothmodels with \textit{Gaia} observations, for a wide variety of environments(galactic nuclei, globular clusters, the Large Magellanic Clouds, etc.).

Hypervelocity Stars from a Supermassive Black Hole-Intermediate-mass Black Hole binary