Table 2: The disruption time and the formation rate of clusters within 600 pc from the Sun for two assumed values of the lower mass limit of clusters in the Kharchenko et al. (2005) sample.
Mass range $\mbox{$t_0$ }$ $\log~(CFR)$ $\log~(CFR)$

( $M_{\odot }$ ) (Myr) Nr/yr $M_{\odot }$ /yr

$8\times 10^1{-}1\times 10^5$ $\rm 3.5^{+1.3}_{-1.0}$ $-6.03\pm 0.02$ $-3.27\pm 0.02$

$1\times10^2{-}1\times 10^5$ $\rm 3.1^{+1.2}_{-0.8}$ $-6.03\pm 0.02$ $-3.19\pm 0.02$

adopted $\rm 3.3^{+1.4}_{-1.0}$ $-6.03\pm 0.02$ $-3.23\pm 0.06$

**Table 2:** The disruption time and the formation rate of clusters within 600 pc from the Sun for two assumed values of the lower mass limit of clusters in the Kharchenko et al. (2005) sample.
Mass range	$\mbox{$t_0$ }$	$\log~(CFR)$	$\log~(CFR)$
( $M_{\odot }$ )	(Myr)	Nr/yr	$M_{\odot }$ /yr
$8\times 10^1{-}1\times 10^5$	$\rm 3.5^{+1.3}_{-1.0}$	$-6.03\pm 0.02$	$-3.27\pm 0.02$
$1\times10^2{-}1\times 10^5$	$\rm 3.1^{+1.2}_{-0.8}$	$-6.03\pm 0.02$	$-3.19\pm 0.02$
adopted	$\rm 3.3^{+1.4}_{-1.0}$	$-6.03\pm 0.02$	$-3.23\pm 0.06$

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