New high precision spectroscopic observations and proper motion studies of thousands of stars in selected Galactic globular clusters are beginning to reveal detailed information about the three-dimensional kinematics of this class of stellar systems. Such a complete view of the velocity space calls for a much more complex dynamical interpretation with respect to the traditional paradigm, in which, for simplicity, the effects of internal rotation are often neglected. In view of this, we present the results of an extensive survey of N-body simulations designed to investigate the long-term dynamical evolution of star clusters characterized by a broad range of different initial structural and kinematical properties, including the presence of differential rotation. We will discuss in detail the role of angular momentum in the evolution toward core collapse by comparing the evolution of rotating and non-rotating stellar systems with similar initial structure. Particular attention will be given to the analysis of the evolution of pressure anisotropy and its radial variation in the simulated star clusters.
|Publication status||Published - 1 Jun 2013|