It is believed that most stars are born in stellar clusters, which
dissolve over time so that the members become part of the disc and halo
population of the Galaxy.
In the present work we will assume that these young stellar clusters
live mainly within the disc of the Galaxy. We have explored four
different primordial binary percentages: 0%, 10% and 50%. We have
quantified the contribution of these escaping stars to the Galaxy
population by analysing their escape velocity and evolutionary stage at
the moment of escape. In this way we could analyse the mechanisms that
produced these escapers, whether evaporation through weak two-body
encounters, energetic close encounters or stellar evolution events, e.g.
supernovae.
We could also infer that dissolving stellar clusters such as those that
we have modeled can populate the Galactic halo with giants stars for
which the progenitors were stars of up to 2.4 M⊙. Furthermore, choices
made for the velocity kicks of remnants do influence the production of
hyper-velocity stars.