Searching for New Observational Signatures of the Dynamical Evolution of Star Clusters

Abstract We present a numerical study, based on Monte Carlo simulations, aimed at defining new empirical parameters measurable from observations and able to trace the different phases of dynamical evolution star clusters. As expected, central density cusp, deviating King model profile, develops during core collapse (CC) event. Although slope varies post-CC oscillations, cusp remains stable feature characterizing portion profile in all stages. then investigate normalized cumulative radial distribution (nCRD) drawn by cluster stars included within one half tridimensional half-mass radius ( R ≤ 0.5 r h ), finding that its morphology time according cluster’s stage. To quantify these changes we defined three parameters: A 5 , area subtended nCRD 5% radius, P value measured same distance, S 2.5 straight line tangent = 2.5% . The evolve similarly evolution: after an early phase which they are essentially constant, their values rapidly increase, reaching maximum CC epoch slightly decreasing phase, when average significantly larger than initial one, spite some fluctuations. results presented this paper suggest observable very promising tools identify stage observational data.