Cluster CMDs from N-body simulations: stellar and binary evolution on GRAPE

The Colour-Magnitude diagram (CMD) is an important observational tool for use in the study of star clusters. Thus it is important to include a consistent treatment of stellar aid binary evolution in N-body codes to allow the generation and interaction of the full range of stellar populations. In this way realistic cluster models can be compared with observed cluster populations via the respective CMDs. Preliminary results of such an approach using the Aarseth NBODY4 code on the CRAPE-6 are presented here. In particular, by using a stellar evolution algorithm that includes metallicity as a free parameter, the stellar populations of clusters at various stages of evolution can be studied. Interesting formation cases directly influenced by the cluster environment are highlighted for various stellar sub-populations.