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Article Contents
1 Introduction
2 A power law expression for the disruption time of star clusters
3 The decrease of the cluster mass due to stellar evolution and tidal effects
4 Comparison of the analytic solution with results of N-body simulations
5 The predicted mass and age distributions of cluster samples
6 Application to Galactic open clusters
7 Discussion and summary

List of tables
List of figures

Copyright ESO 2005
Published by EDP Sciences