Abstract
The dynamical role of stellar evolution in globular clusters is explored using simple models. The cluster initial mass function is divided into mass groups spanning the range 4.0 - 0.35 M_sun;. The evolution of the cluster is calculated incorporating the modification of the mass function by stellar evolution, the weakening of the cluster potential due to the escape of shed stellar mass from the cluster, the collisional transfer of energy between the various mass groups, and evaporation. It is found that the dynamical evolution of clusters born rich in massive stars or with long initial relaxation times is dominated by stellar mass loss. Massive clusters of this type will have long pre-core collapse lives. Clusters born poor in massive stars or with short initial relaxation times are dominated by collisional evolution; the role of stellar evolution in these systems is to delay core collapse. These clusters suffer rapid core collapse, typically in 1 - 5 Gyr.
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