Abstract
Abstract.If the cluster formation rate is constant and the disruption time of clusters depends on their initial mass as \(t_{\rm dis} = t_4 \times (M_{\rm cl}/10^4 M_\odot)^\gamma\), the values of t 4 and \(\gamma\) can be derived in a very simple way from the age and mass histograms of large homogeneous samples of clusters with reliable age and/or mass determinations. We demonstrate the method and derive the values of t 4 and \(\gamma\) from cluster samples in selected fields of four galaxies: M51, M33, SMC and the solar neighbourhood. The values of \(\gamma\) are the same within their uncertainties in the four galaxies with \( < \gamma > = 0.62 \pm 0.06\). However, the disruption time t 4 of clusters of \(10^4 M_\odot\) is very different in the different locations. It is shortest in the inner region of M51 ( t 4 = 4 x 107 yrs) and highest in the SMC ( t 4 = 4 x 109 yrs).
Published Version
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