In this study , we characterized 16 objects previously classified as faint or low contrast Galactic open clusters ( OCs ) .
We employed parameters associated to the OCs dynamical evolution : core ( r _ { c } ) , tidal ( r _ { t } ) and half-mass ( r _ { hm } ) radii , age and crossing time ( t _ { cr } ) .
Relations among these parameters were exploited to draw some evolutionary connections .
We also included 11 OCs with previous characterizations to provide wider coverage of the parameters space .
The investigated sample spans a considerable range in age ( log ( t yr ^ { -1 } ) \sim 7.0 - 9.7 ) and Galactocentric distance ( R _ { G } \sim 6 - 11 kpc ) .
Most of them present solar metallicity .
We employed GAIA DR2 astrometry and photometry and selected member stars through a decontamination algorithm which explores the 3D astrometric space ( \mu _ { \alpha } , \mu _ { \delta } , \varpi ) to assign membership likelihoods .
Previous studies of most of these objects were based mostly on photometric information .
All investigated OCs were proved to be real stellar concentrations and relations among their parameters indicate a general disruption scenario in which OCs tend to be more concentrated as they evolve .
Internal interactions sucessively drive OCs to develop more dynamically relaxed structures and make them less subject to mass loss due to tidal effects .
Tidal radius tends to increase with R _ { G } in accordance with the strength of the Galactic tidal field .
Besides , the correlation between the r _ { c } and the dynamical ratio \tau _ { \textrm { dyn } } = \textrm { age } / t _ { cr } suggests two distinct evolutionary sequences , which may be consequence of different initial formation conditions .