Star Cluster Evolution, Dynamical Age Estimation and the Kinematical Signature of Star Formation K3

We distribute 400 stars in N bin = 200 binary systems in clusters with initial half mass radii 0.077 ≤ R 0.5 ≤ 2.53 pc and follow the subsequent evolution of the stellar systems by direct N-body integration. The stellar masses are initially paired at random from the KTG(1.3) initial stellar mass function. The initial period distribution is flat ranging from… CONTINUE READING