1996A&A...308..141D

N-body simulations of open clusters with several different initial mass functions (IMFs) have been performed in order to study their influence on the dynamical evolution of clusters. These simulations differ from those presented in Paper I (de la Fuente Marcos 1995) in that they consider clusters with mass loss due to stellar evolution. The results show that for all the IMFs studied the evolution of the cluster is slowed down and the initial core collapse loses importance due to an expansion of the inner regions of the cluster. We find that the total disruption time is very IMF dependent because of different numbers of massive stars and also it depends on the richness of the cluster. Some questions concerning mass loss and formation of multiple systems are discussed briefly.