  We carry out a search for tidal tails in a sample of open clusters with known
relatively elongated morphology. We identify the member stars of these clusters
from the precise astrometric and deep photometric data from $Gaia$ Early Data
Release 3 using the robust membership determination algorithm, ML-MOC. We
identify 46 open clusters having a stellar corona beyond the tidal radius, 20
of which exhibit extended tails aligned with the cluster orbit direction in
galactocentric coordinates. Notably we find NGC 6940 (at a distance of $\sim1$
kpc) is the furthest open cluster exhibiting tidal tails that are $\sim50$ pc
from its center, while also identifying $\sim40$ pc long tidal tails for the
nearby Pleiades. Using the minimum spanning tree length for the most massive
stars relative to all cluster members, we obtain the mass segregation ratio
($\rm\lambda_{MSR}$) profiles as a function of the number of massive stars in
each cluster. From these profiles, we can classify the open clusters into four
classes based on the degree of mass segregation experienced by the clusters. We
find that clusters in the most mass segregated classes are the oldest on
average and have the flattest mass function slope. Of the 46 open clusters
studied in this work, 41 exhibit some degree of mass segregation. Furthermore,
we estimate the initial masses (M$\rm_{i}$) of these open clusters finding that
some of them, having M$\rm_{i}\gtrsim 10^{4} M_{\odot}$, could be the
dissolving remnants of Young Massive Clusters.
