Abstract
We study the evolution and observability of young and compact star clusters near the Galactic center, such as the Arches cluster and the Quintuplet. The star clusters are modeled with a combination of techniques; using direct N-body integration to calculate the motions of all stars and detailed stellar and binary evolution to follow the evolution of the stars. The modeled star clusters dissolve within 10 to 60 million years in the tidal field of the Galaxy. The projected stellar density in the modeled clusters drops within 5% to 70% of the lifetime to a level comparable to the projected background density towards the Galactic center. We therefore conclude that between 20 and 50 clusters with characteristics similar to the Arches and the Quintuplet cluster exist. At young age these clusters are highly collisional. This leads to the build-up of a massive collision runaway in each of these clusters. The mass of the collision runaway easily exceeds several hundred M⊙, and the star will be rotating close to br...
Published Version
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