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Globular clusters (GCs) and many nuclear clusters (NCs) show evidence forhosting multiple generations of stellar populations. Younger stellarpopulations in NCs appear to reside in disk like structures, including thenuclear cluster in our own Galactic center as well as in M31. Kinematic studiesof the anomalous globular cluster Omega Centauri, thought to possibly be aformer dwarf galaxy (or a galactic nucleus), show evidence for its hosting of acentral, kinematically cold disk component. These observations suggest thatformation of second (or multiple) generation stars may occur in flattened disklike structures. Here we use detailed N-body simulations to explore thepossible evolution of such stellar disks, embedded in globular clusters. Wefollow the long term evolution of a disk like structure similar to thatobserved in Omega Centauri and study its properties. We find that astellar-disk like origin for second generation stellar populations can leavebehind significant kinematic signatures in properties of the clusters,including an anisotropic distribution, and lower velocity dispersions, whichcan be used to constrain the origin of second generations stars and theirdynamical evolution.

Evolution of second generation stars in stellar disks of globular and nuclear clusters: Omega Centauri as a test case