N-Body simulations of compact young clusters near the galactic center

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dc.contributor.author Kim, Sungsoo en_US
dc.contributor.author Figer, Donald en_US
dc.contributor.author Lee, Hyung Mok en_US
dc.contributor.author Morris, Mark en_US
dc.date.accessioned 2006-06-12T14:05:37Z en_US
dc.date.available 2006-06-12T14:05:37Z en_US
dc.date.issued 2000-12-10 en_US
dc.identifier.citation Astrophysical Journal 545N1 (2000) 301-308 en_US
dc.identifier.issn 1538-4357 en_US
dc.identifier.uri http://hdl.handle.net/1850/1986 en_US
dc.description Also archived in: arXiv:astro-ph/0008441 v1 28 Aug 2000 en_US
dc.description.abstract We investigate the dynamical evolution of compact young star clusters (CYCs) near the Galactic center (GC) using Aarseth’s Nbody6 codes. The relatively small number of stars in the cluster (5,000–20,000) makes real-number N-body simulations for these clusters feasible on current workstations. Using Fokker-Planck (F-P) models, Kim, Morris, & Lee (1999) have made a survey of cluster lifetimes for various initial conditions, and have found that clusters with a mass ∼ < 2 × 104M⊙ evaporate in ∼ 10 Myr. These results were, however, to be confirmed by N-body simulations because some extreme cluster conditions, such as strong tidal forces and a large stellar mass range participating in the dynamical evolution, might violate assumptions made in F-P models. Here we find that, in most cases, the CYC lifetimes of previous F-P calculations are 5–30% shorter than those from the present N-body simulations. The comparison of projected number density profiles and stellar mass functions between N-body simulations and HST/NICMOS observations by Figer et al. (1999) suggests that the current tidal radius of the Arches cluster is ∼ 1.0 pc, and the following parameters for the initial conditions of that cluster: total mass of 2 × 104M⊙ and mass function slope for intermediate-to-massive stars of 1.75 (the Salpeter function has 2.35). We also find that the lower stellar mass limit, the presence of primordial binaries, the amount of initial mass segregation, and the choice of initial density profile (King or Plummer models) do not significantly affect the dynamical evolution of CYCs. (Refer to PDF file for exact formulas). en_US
dc.description.sponsorship This work was partially supported by a NASA grant to UCLA, and H.M.L. acknowledges the support from the KOSEF through grant 1999-2-113-001-5. en_US
dc.format.extent 198393 bytes en_US
dc.format.mimetype application/pdf en_US
dc.language.iso en_US en_US
dc.publisher University of Chicago Press: Astrophysical Journal en_US
dc.relation.ispartofseries vol. 545 en_US
dc.relation.ispartofseries no. 1 en_US
dc.relation.ispartofseries part 1 en_US
dc.relation.ispartofseries pps. 301-308 en_US
dc.subject Celestial mechanics en_US
dc.subject Galaxies-center en_US
dc.subject Galaxies-star clusters en_US
dc.subject Methods-n-body simulations en_US
dc.subject Stars-clusters en_US
dc.subject Stellar dynamics en_US
dc.title N-Body simulations of compact young clusters near the galactic center en_US
dc.type Preprint en_US

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