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Paper: Theoretical and Observational Agreement on Mass Dependence of Cluster Life Times
Volume: 322, The Formation and Evolution of Massive Young Star Clusters
Page: 481
Authors: Gieles, M.; Baumgardt, H.; Bastian, N.; Lamers, H.J.G.L.M.
Abstract: Observations and N-body simulations both support a simple relation for the disruption time of a cluster as a function of its mass of the form: tdis = t4 × (M/104MSolar)γ. The scaling factor t4 seems to depend strongly on the environment. Predictions and observations show that γ ≈ 0.64 ± 0.06. Assuming that tdisM0.64 is caused by evaporation and shocking implies a relation between the radius and the mass of a cluster of the form: rhM0.07, which has been observed in a few galaxies. The suggested relation for the disruption time implies that the lower mass end of the cluster initial mass function will be disrupted faster than the higher mass end, which is needed to evolve a young power law shaped mass function into the log-normal mass function of old (globular) clusters.
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