The effect of secular galactic growth on the evolution of star clusters

Abstract

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.

MNRAS accepted

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Cited by in corpus (6)

• Stellar-mass black holes in young massive and open stellar clusters and their role in gravitational-wave generation
• The origin of the Milky Way globular clusters
• Evolution of star cluster systems in isolated galaxies: first results from direct $N$-body simulations
• A tight relation between the age distributions of stellar clusters and the properties of the interstellar medium in the host galaxy
• The properties, origin and evolution of stellar clusters in galaxy simulations and observations
• The contribution of dissolving star clusters to the population of ultra-faint objects in the outer halo of the Milky Way