  We present the dynamical evolution of ten open clusters which were part of
our previous studies. These clusters include both young and intermediate-age
open clusters with ages ranging from 25$\pm$19 Myr to 1.78$\pm$0.20 Gyr. The
total mass of these clusters ranges from 356.18$\pm$142.90 to
1811.75$\pm$901.03 M$_{\odot}$. The Galactocentric distances to the clusters
are in the range of 8.91$\pm$0.02 to 11.74$\pm$0.18 kpc. The study is based on
the ground-based UBVRI data supplemented by the astrometric data from the Gaia
archive. We studied the minimum spanning tree of the member stars for these
clusters. The mass segregation in these clusters was quantified by mass
segregation ratios calculated from the mean edge length obtained through the
minimum spanning tree. The clusters NGC 2360, NGC 1960, IC 1442, King 21, and
SAI 35 have ${\Gamma}_{MSR}$ to be 1.65$\pm$0.18, 1.94$\pm$0.22, 2.21$\pm$0.20,
1.84$\pm$0.23, and 1.96$\pm$0.25, respectively which indicate moderate mass
segregation in these clusters. The remaining five clusters are found to exhibit
weak or no mass segregation. We used the ratio of half mass radius to the tidal
radius i.e. R$_{h}$/R$_{t}$ to investigate the effect of the tidal interactions
on the cluster structure and dynamics. The ratios of half mass radii to tidal
radii are found to be positively correlated with the Galactocentric distances
with a linear slope of 0.06$\pm$0.01 having linear regression coefficient
r-square = 0.93 for the clusters.

Astrophysics of Galaxies;Solar and Stellar Astrophysics