Theoretical and observational agreement on mass dependence of cluster life times

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.

References(3)

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Dynamical evolution of star clusters in tidal fields

- Mon.Not.Roy.Astron.Soc. 340 (2003) 227
•
e-Print:
- astro-ph/0211471
•
DOI:
- 10.1046/j.1365-8711.2003.06286.x

Star cluster formation and disruption time-scales - I. an empirical determination of the disruption time of star clusters in four galaxies

- Mon.Not.Roy.Astron.Soc. 338 (2003) 717
•
e-Print:
- astro-ph/0210595
•
DOI:
- 10.1046/j.1365-8711.2003.06083.x

The formation and evolution of young globular clusters in ngc 3256

- Astron.J. 118 (1999) 752
•
e-Print:
- astro-ph/9904247
•
DOI:
- 10.1086/300961