Abstract
If the cluster formation rate is constant and the disruption time of clusters depends only on their initial mass as tdis = t4 × (Mcl/104M⊙)γ, the values of t4 and γ can be derived in a very simple way from the age and mass histograms of observed clusters. We derived these values from cluster samples in fields of five galaxies: M51, M33, LMC, SMC and the solar neighbourhood. The values of γ are the same in the five galaxies with < γ > = 0.62 ± 0.03. However the disruption time t4 of clusters of 104M⊙ is very different in the different locations.
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