  Interacting galaxies favor the formation of star clusters but are also
suspected to affect their evolution through an intense and rapidly varying
tidal field. Treating this complex behaviour remains out-of-reach of
(semi-)analytical studies. By computing the tidal field from galactic models
and including it into star-by-star N-body simulations of star clusters, we
monitor the structure and mass evolution of a population of clusters in a
galaxy major merger, taking the Antennae galaxies (NGC 4038/39) as a prototype.
On the long timescale (~ 10^9 yr), the merger only indirectly affects the
evolution of clusters by modifying their orbits in or around the galaxies: the
mass-loss of clusters in the merger remnant is faster, while clusters ejected
in the tidal debris survive much longer, compared to in an isolated galaxy. The
tidal perturbations of the galactic collisions themselves are too short lived
and not strong enough to significantly influence the structure and dissolution
of realistically dense/massive star clusters.
