Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 458, Issue 2, Pages 1450-1465Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw274
Keywords
methods: numerical; stars: black holes; stars: kinematics and dynamics; globular clusters: general
Categories
Funding
- Silk Road Project at the National Astronomical Observatories of China (NAOC)
- Max-Planck Computing and Data Facility (MPCDF) in Garching, Germany
- 'Alexander von Humboldt Polish Honorary Research Fellowship' by the Foundation for Polish Science
- Volkswagen Trilateral Partnership grant [90411]
- Nicolaus Copernicus Astronomical Center, Warsaw, Poland
- Chinese Academy of Sciences at the NAOC [2009S1-5]
- 'Qianren' special foreign experts programme of China at the NAOC
- Polish Ministry of Sciences and Higher Education [DEC-2012/07/B/ST9/04412]
- Nicolaus Copernicus Astronomical Center's grant for young researchers
- MPCDF cluster of excellence Origin and Structure of the Universe
- Peter and Patricia Gruber Foundation through the PPGF Fellowship
- Peking University One Hundred Talent Fund (985)
- National Natural Science Foundation of China [11050110414, 11173004, 11573004]
Ask authors/readers for more resources
Introducing the dragon simulation project, we present directN-body simulations of four massive globular clusters (GCs) with 10(6) stars and 5 per cent primordial binaries at a high level of accuracy and realism. The GC evolution is computed with nbody6++gpu and follows the dynamical and stellar evolution of individual stars and binaries, kicks of neutron stars and black holes (BHs), and the effect of a tidal field. We investigate the evolution of the luminous (stellar) and dark (faint stars and stellar remnants) GC components and create mock observations of the simulations (i.e. photometry, colour-magnitude diagrams, surface brightness and velocity dispersion profiles). By connecting internal processes to observable features, we highlight the formation of a long-lived 'dark' nuclear subsystem made of BHs, which results in a two-component structure. The inner core is dominated by the BH subsystem and experiences a core-collapse phase within the first Gyr. It can be detected in the stellar (luminous) line-of-sight velocity dispersion profiles. The outer extended core - commonly observed in the (luminous) surface brightness profiles - shows no collapse features and is continuously expanding. We demonstrate how a King model fit to observed clusters might help identify the presence of post core-collapse BH subsystems. For global observables like core and half-mass radii, the direct simulations agree well with Monte Carlo models. Variations in the initial mass function can result in significantly different GC properties (e.g. density distributions) driven by varying amounts of early mass-loss and the number of forming BHs.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available