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Globular Clusters (GCs) and Nuclear Star Clusters (NSCs) are typicallycomposed by several stellar populations, characterized by different chemicalcompositions. Different populations show different ages in NSCs but notnecessarily in GCs. The youngest populations in NSCs appear to reside indisk-like structures, as observed in our Galaxy and in M31. Gas infall followedby formation of second generation (SG) stars in GCs may similarly formdisk-like structures in the clusters nuclei. Here we explore this possibilityand follow the long term evolution of stellar disks embedded in GCs, and studytheir effects on the evolution of the clusters. We study disks with differentmasses by means of detailed N-body simulations and explore their morphologicaland kinematic signatures on the GC structures. We find that as a secondgeneration disk relaxes, the old, first generation, stellar population flattensand becomes more radially anisotropic, making the GC structure become moreelliptical. The second generation stellar population is characterized by alower velocity dispersion, and a higher rotational velocity, compared with theprimordial older population. The strength of these kinematic signatures dependsboth on the relaxation time of the system and on the fractional mass of thesecond generation disk. We therefore conclude that SG populations formed inflattened configurations will give rise to two systematic trends: (1) Positivecorrelation between GC ellipticity and fraction of SG population (2) Positivecorrelation between GC relaxation time and ellipticity. Thereby GCellipticities and rotation could be related to the formation of SG stars andtheir initial configuration.

Second generation stellar disks in Dense Star Clusters and cluster ellipticities