  The sedimentation level of blue straggler stars (BSS) has been shown to be a
great tool to investigate the dynamical states of globular clusters (GCs). The
area enclosed between the cumulative radial distributions of BSS and a
reference population up to the half-mass radius of the clusters,
$A^+_{\mathrm{rh}}$, is known to be a measure of the sedimentation of BSS in
GCs. In this work, we calculate $A^+_{\mathrm{rh}}$ for 12 open clusters (OCs)
using main-sequence turn-off stars as a reference population. The BSS as well
as the main-sequence turn-off stars for these clusters are identified using the
proper motions and parallaxes from the Gaia DR2 data, with spectroscopically
confirmed BSS populations for some of these clusters available in the
literature. Using the Pearson and Spearman rank correlation coefficients, we
find weak correlations between the estimated values of $A^+_{\mathrm{rh}}$ and
other markers of dynamical ages of the clusters, i.e., the number of central
relaxations a cluster has experienced since its formation, and the structural
parameters of the clusters. Based on statistical tests, we find that these
correlations are similar to the corresponding correlations among the less
evolved GCs, albeit within large errors.
