Recent spectroscopic observational studies have provided evidence that young massive star clusters can be characterized by a significant amount of internal rotation. Such evidence calls for renewed efforts in the investigation of the role of angular momentum in the formation and early stages of dynamical evolution of star clusters. We performed a survey of N-body simulations to follow the dynamics of the collapse of stellar systems with different initial values of total angular momentum and global virial ratio. We present here the preliminary results of simulations starting from initial conditions characterized by different degrees of departure from spatial homogeneity and approximate solid-body rotation. We describe the dynamical properties of the final equilibrium configurations, with particular attention to the effects of internal rotation on the dynamical evolution of the early substructures.
|Publication status||Published - 1 Jun 2013|