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A comprehensive Nbody study of mass segregation in star clusters : Energy equipartition and ejection

We address the dynamical evolution of an isolated self–gravitating system with two stellar mass groups. We vary the individual ratio of the heavy to light bodies, µ from 1.25 to 50 and alter also the fraction of the total heavy mass M h from 5% to 40% of the whole cluster mass. Clean-cut properties of the cluster dynamics are examined, like core collapse, the evolution of the central potential, as well as escapers. We present in this work collisional N-body simulations, using the high–order integrator NBODY6++ with up to N ⋆ = 2 · 10 4 particles improving the statistical significancy of the lower– N ⋆ simulations by ensemble averages. Equipartition slows down the gravothermal contraction of the core slightly. Beyond a critical value of µ ≈ 2, no equipartition can be achieved between the different masses; the heavy component decouples and collapses. For the first time the critical boundary between Spitzer–stable and –unstable systems is demonstrated in direct N-body models.