  The growth of galaxies through adiabatic accretion of dark matter is one of
the main drivers of galaxy evolution. By isolating it from other processes like
mergers, we analyse how it affects the evolution of star clusters. Our study
comprises a fast and approximate exploration of the orbital and intrinsic
cluster parameter space, and more detailed monitoring of their evolution,
through N-body simulations for a handful of cases. We find that the properties
of present-day star clusters and their tidal tails differ very little, whether
the clusters are embedded in a growing galactic halo for 12 Gyr, or in a static
one.
