Self-consistent simulations of star cluster formation from gas clouds under the influence of galaxy-scale tidal fields

Abstract

We present the first results of a project aimed at following the formation and long-term dynamical evolution of star clusters within the potential of a host galaxy. Here we focus on a model evolved within a simplified potential representing the Large Magellanic Cloud. This demonstrates for the first time the self-consistent formation of a bound star cluster from a giant molecular cloud. The model cluster reproduces the density profiles and structural characteristics of observed star clusters.

5 pages, 3 figures, accepted for publication in MNRAS Letters

References in corpus (14)

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Cited by in corpus (14)

• A New Method for Estimating Dark Matter Halo Masses using Globular Cluster Systems
• On the evolution of a star cluster and its multiple stellar systems following gas dispersal
• Secondary star formation within massive star clusters: Origin of multiple stellar populations in globular clusters
• The bound fraction of young star clusters
• Black hole mergers in compact star clusters and massive black hole formation beyond the mass-gap
• The Size Scale of Star Clusters
• On the origin of double main-sequence turn-offs in star clusters of the Magellanic Clouds
• Evolution of star cluster systems in isolated galaxies: first results from direct $N$-body simulations
• Globular cluster formation with multiple stellar populations: self-enrichment in fractal massive molecular clouds
• From hydrodynamics to N-body simulations of star clusters: mergers and rotation
• Star cluster dynamics
• Formation of globular clusters with multiple stellar populations from massive gas clumps in high-z gas-rich dwarf galaxies
• The properties, origin and evolution of stellar clusters in galaxy simulations and observations
• On the Survival of High-Altitude Open Clusters within the Milky Way Galaxy Tides