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The Disruption Time of Clusters in Different Galaxies

Published online by Cambridge University Press:  03 August 2017

Stratos G. Boutloukos  and
Henny J.G.L.M. Lamers
Stratos G. Boutloukos
Affiliation:
Aristotle University, Thessaloniki, Greece Astronomical Institute
Henny J.G.L.M. Lamers
Affiliation:
Astronomical Institute SRON Laboratory for Space Research, Utrecht University, Princetonplein 5, NL-3584CC, Utrecht, the Netherlands

Abstract

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If the cluster formation rate is constant and the disruption time of clusters depends only on their initial mass as t dis = t 4 × (M cl/104M ⊙)γ, the values of t 4 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 t 4 of clusters of 104M ⊙ is very different in the different locations.

Information

Type
Part 4. Star Cluster Formation and Evolution: Theory and Observation
Information
Symposium - International Astronomical Union , Volume 207: Extragalactic Star Clusters , 2002 , pp. 703 - 705
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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