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In this paper we use N-body simulations to study the effects of primordialmass segregation on the early and long-term evolution of star clusters. Oursimulations show that in segregated clusters early mass loss due to stellarevolution triggers a stronger expansion than for unsegregated clusters. Tidallylimited, strongly segregated clusters may dissolve rapidly as a consequence ofthis early expansion, while segregated clusters initially underfilling theirRoche lobe can survive the early expansion and have a lifetime similar to thatof unsegregated clusters. Long-lived initially segregated clusters tend to havelooser structure and reach core collapse later in their evolution thaninitially unsegregated clusters. We have also compared the effects of dynamicalevolution on the global stellar mass function (MF) of low-mass main sequencestars. In all cases the MF flattens as the cluster loses stars. The amount ofMF flattening induced by a given amount of mass loss in a rapidly dissolvinginitially segregated cluster is less than for an unsegregated cluster. Theevolution of the MF of a long-lived segregated cluster, on the other hand, isvery similar to that of an initially unsegregated cluster.

Effects of Primordial Mass Segregation on the Dynamical Evolution of Star Clusters