Table 1: Approximations to the mass lost by stellar evolution for ${\it GALEV}$ cluster models with a Salpeter IMF of $\alpha =-2.35$ , $0.15 < M_* < 85~\mbox{$M_{\odot}$ }$ and 0.0004<Z<0.05.
Z $a_{\rm ev}$ $b_{\rm ev}$ $c_{\rm ev}$

0.0004 7.06 0.265 -1.790

0.0040 7.06 0.260 -1.800

0.0080 7.03 0.260 -1.800

0.0200 7.00 0.255 -1.805

0.0500 7.00 0.250 -1.820

**Table 1:** Approximations to the mass lost by stellar evolution for ${\it GALEV}$ cluster models with a Salpeter IMF of $\alpha =-2.35$ , $0.15 < M_* < 85~\mbox{$M_{\odot}$ }$ and 0.0004<Z<0.05.
Z	$a_{\rm ev}$	$b_{\rm ev}$	$c_{\rm ev}$
0.0004	7.06	0.265	-1.790
0.0040	7.06	0.260	-1.800
0.0080	7.03	0.260	-1.800
0.0200	7.00	0.255	-1.805
0.0500	7.00	0.250	-1.820

Source LaTeX | All tables | In the text

	1 Introduction
	2 A power law expression for the disruption time of star clusters
	3 The decrease of the cluster mass due to stellar evolution and tidal effects
	4 Comparison of the analytic solution with results of N-body simulations
	5 The predicted mass and age distributions of cluster samples
	6 Application to Galactic open clusters
	7 Discussion and summary
	References