Million-body star cluster simulations

• Verfasst von: Rodriguez, Carl L. [VerfasserIn]
• Verfasst von: Spurzem, Rainer [VerfasserIn]
• Titel: Million-body star cluster simulations
• Titelzusatz: comparisons between Monte Carlo and direct N-body
• Verf.angabe: Carl L. Rodriguez, Meagan Morscher, Long Wang, Sourav Chatterjee, Frederic A. Rasio and Rainer Spurzem
• E-Jahr: 2016
• Jahr: 24 August 2016
• Umfang: 10 S.
• Fussnoten: Gesehen am 27.10.2017
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2016
• Band/Heft Quelle: 463(2016), 2, Seite 2109-2118
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stw2121
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1564840999

Abstract

We present the first detailed comparison between million-body globular cluster simulations computed with a Hénon-type Monte Carlo code, cmc, and a direct N-body code, nbody6++gpu. Both simulations start from an identical cluster model with 106 particles, and include all of the relevant physics needed to treat the system in a highly realistic way. With the two codes ‘frozen’ (no fine-tuning of any free parameters or internal algorithms of the codes) we find good agreement in the overall evolution of the two models. Furthermore, we find that in both models, large numbers of stellar-mass black holes (>1000) are retained for 12 Gyr. Thus, the very accurate direct N-body approach confirms recent predictions that black holes can be retained in present-day, old globular clusters. We find only minor disagreements between the two models and attribute these to the small-N dynamics driving the evolution of the cluster core for which the Monte Carlo assumptions are less ideal. Based on the overwhelming general agreement between the two models computed using these vastly different techniques, we conclude that our Monte Carlo approach, which is more approximate, but dramatically faster compared to the direct N-body, is capable of producing an accurate description of the long-term evolution of massive globular clusters even when the clusters contain large populations of stellar-mass black holes.