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The capability to reconstruct dissolved stellar systems in dynamical andchemical space is a key factor in improving our understanding of the evolutionof the Milky Way. Here we concentrate on the dynamical aspect and given that asignificant portion of the stars in the Milky Way have been born in stellarassociations or clusters that have lived a few Myr up to several Gyr, wefurther restrict our attention to the evolution of star clusters. We havecarried out our simulations in two steps: (1) we create a simulation ofdissolution and mixing processes which yields a close fit to the present-dayMilky Way dynamics and (2) we have evolved three sets of stellar clusters withmasses of 400, 1000 and 15000 M$_{\odot}$ to dissolution. The birth location ofthese sets was 4, 6, 8 and 10 kpc for the 400 and 1000 M$_{\odot}$ clusters and4, 6, 8, 10 and 12 kpc for the 15000 M$_{\odot}$. We have focused our effortson studying the state of the escapers from these clusters after 4.5 Gyr ofevolution with particular attention to stars that reach the Solar annulus, i.e.7.5 $\le$ R$_{\rm{gc}}$ $\le$ 8.5 kpc. We give results for Solar twins andsiblings over a wide range of radii and cluster masses for two dissolutionmechanisms. From kinematics alone, we conclude that the Sun was $\sim$50 percent more likely to have been born near its current Galactocentric radius,rather than have migrated (radially) $\sim$2 kpc since birth. We conclude ouranalysis by calculating magnitudes and colours of our single stars forcomparison with the samples that the $Gaia$, $Gaia$-ESO and GALAH-AAO surveyswill obtain. In terms of reconstructing dissolved star clusters we find that onshort time-scales we cannot rely on kinematic evolution alone and thus it willbe necessary to extend our study to include information on chemical space.

Tracking Cluster Debris (TraCD)- I. Dissolution of clusters and searching the solar cradle