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The survival time of a star cluster depends on its total mass, density, andthus size, as well as on the environment in which it was born and in whichlies. Its dynamical evolution is influenced by various factors such asgravitational effects of the Galactic bar, spiral structures, and molecularclouds. Overall, the factors that determine the longevity of a cluster arecomplex and not fully understood. This study aims to investigate if openclusters and field stars respond differently to the perturbations that causeradial migration. In particular, we aim at understanding the nature of theoldest surviving clusters. We compared the time evolution of the kinematicproperties of two Gaia DR3 samples: the first sample is composed of $\sim$40open clusters and the second one of $\sim$66,000 MSTO field stars. Bothselected samples are composed of stars selected with the same qualitycriterion, belonging to the thin disc, in a similar metallicity range, locatedin the same Galactocentric region [7.5-9 kpc] and with ages >1 Gyr. Weperformed a statistical analysis comparing the properties of the samples offield stars and of open clusters. A qualitative comparison of kinematic andorbital properties reveals that clusters younger than 2-3 Gyr are moreresistant to perturbations than field stars and they move along quasi-circularorbits. Conversely, clusters older than approximately 3 Gyr have more eccentricand inclined orbits than isolated stars in the same age range. Such orbits leadthem to reach higher elevations on the Galactic plane, maximising theirprobability to survive several Gyr longer. A formal statistical analysisreveals that there are differences among the time evolution of most of thekinematic and orbital properties of field stars and open clusters. Our resultssuggest that oldest survived clusters are usually more massive and move onorbits with higher eccentricity.

The role of radial migration in open cluster and field star populations with Gaia dr3