• DOI:10.1093/mnras/stt1351
• Corpus ID: 54177579

Mergers of multimetallic globular clusters: the role of dynamics

@article{AmaroSeoane2011MergersOM,
  title={Mergers of multimetallic globular clusters: the role of dynamics},
  author={Pau Amaro-Seoane and Symeon Konstantinidis and Patrick Brem and M{\'a}rcio Catel{\'a}n},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2011},
  volume={435},
  pages={809-821}
}

• P. Amaro-Seoane, Symeon Konstantinidis, +1 author M. Catelán
• Published 25 August 2011
• Physics
• Monthly Notices of the Royal Astronomical Society

Hubble Space Telescope observations of globular clusters (GCs) in the Antenn galaxy show clusters of clusters, or regions in the galaxy that span hundreds of parsecs, where many of the GCs are doomed to collide, and eventually merge. Several such objects appear likely to present a signicant range in ages, hence possibly metallicities, and their merger could plausibly lead to multi-metallic GCs. Here we explore this process with direct-summation N body simulations with GPU hardware. Our results reveal that colliding GCs with dierent metallicities and ages can produce a GC with multiplicity and occupation fractions not unlike those observed in multi-metallic clusters. In our simulations, the merged clusters have a phase with a larger amount of attening than average, as a consequence of rapid rotation { thus suggesting that relatively recent mergers may play a role in producing highly attened, multi-metallic clusters. We additionally explore the role of the King parameter of the cluster in the occupation fractions with a set of 160 direct-summation simulations and nd that for equal size clusters the King parameter of the progenitor clusters determines the occupation fractions in the merger product, while in unequal size mergers the size of the clusters dominates the distribution of stars in the new GC. In particular, we nd that the observed distribution of populations in ! Cen can be described to some extent with our dynamical models.