Mergers of multimetallic globular clusters: the role of dynamics
Hubble Space Telescope observations of globular clusters (GCs) in the Antennae galaxy show clusters of clusters, or regions in the galaxy that span hundreds of parsec, where many of the GCs are doomed to collide, and eventually merge. Several such objects appear likely to present a significant range...
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| Main Authors: | , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
14 August 2013
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2013, Volume: 435, Issue: 1, Pages: 809-821 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stt1351 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stt1351
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| Author Notes: | Pau Amaro-Seoane, Symeon Konstantinidis, Patrick Brem and Márcio Catelan |
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| 520 | |a Hubble Space Telescope observations of globular clusters (GCs) in the Antennae galaxy show clusters of clusters, or regions in the galaxy that span hundreds of parsec, where many of the GCs are doomed to collide, and eventually merge. Several such objects appear likely to present a significant range in ages, hence possibly metallicities, and their merger could plausibly lead to multimetallic GCs. Here we explore this process with direct-summation N-body simulations with graphics processing unit hardware. Our results reveal that colliding GCs with different metallicities and ages can produce a GC with multiplicity and occupation fractions not unlike those observed in multimetallic clusters. In our simulations, the merged clusters have a phase with a larger amount of flattening than average, as a consequence of rapid rotation - thus suggesting that relatively recent mergers may play a role in producing highly flattened, multimetallic 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 find 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 find that the observed distribution of populations in ω Cen can be described to some extent with our dynamical models. | ||
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