Computational methods for collisional stellar systems

Abstract Dense star clusters are spectacular self-gravitating stellar systems in our Galaxy and across the Universe—in many respects. They populate disks spheroids of galaxies as well almost every galactic center. In massive elliptical nuclear harbor supermassive black holes, which might influence evolution their host a whole. The dense is not only governed by aging populations simple Newtonian dynamics. For increasing particle number, unique gravitational effects collisional many-body begin to dominate early cluster evolution. As result, densities become so high that stars can interact collide, binary change dynamical evolution, holes accumulate centers merge with relativistic becoming important. Recent high-resolution imaging has revealed even more complex structural properties respect populations, fractions compact objects as—the still controversial—existence intermediate mass mass. therefore ideal laboratory for concomitant study Not formation disruption be considered but also environments terms initial conditions impact on This review deals specific computational challenges modelling dense, gravothermal clusters.