The disruption time scales of clusters in different galaxies

Details The disruption time scales of clusters in different galaxies The disruption time scales of clusters in different galaxies

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..322..409l&link_type=abstract

The Formation and Evolution of Massive Young Star Clusters, ASP Conference Series, Vol. 322. Edited by H.J.G.L.M. Lamers, L.J.

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Scientific paper

We discuss old and new methods for deriving the disruption times of star clusters from magnitude limited cluster samples. This takes into account the decrease in luminosity and mass due to stellar evolution and disruption. The results agree very well with N-body simulations. Studies of star cluster samples in the solar neighbourhood, SMC, M33 and M51 and comparison with N-body simulations show that the disruption time of star clusters depends on their initial mass as tdis=tenv (Mi/ M&sun;)0.62 and tenv depends on the ambient density as tenv≃ Cenv (ρamb/M&sun; {pc}-3) with Cenv≃ 300 to 800 Myr, except for M51 (and possibly other starburst or interacting galaxies) which has a much shorter disruption time.

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