Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-03-10
Astronomy and Astrophysics
Astrophysics
2 pages, to appear in "The Formation and Evolution of Massive Young Star Clusters", 17-21 November 2003, Cancun (Mexico)
Scientific paper
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: t_dis = t_4 * (M/10^4 Msun)^gamma. The scaling factor t_4 seems to depend strongly on the environment. Predictions and observations show that gamma ~ 0.64 +/- 0.06. Assuming that t_dis ~ M^0.64 is caused by evaporation and shocking implies a relation between the radius and the mass of a cluster of the form: r_h ~ M^0.07, 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.
Bastian Nate
Baumgardt Holger
Gieles Mark
Lamers Henny J. G. L. M.
No associations
LandOfFree
Theoretical and Observational Agreement on Mass Dependence of Cluster Life Times does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Theoretical and Observational Agreement on Mass Dependence of Cluster Life Times, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Theoretical and Observational Agreement on Mass Dependence of Cluster Life Times will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-417892