How well do STARLAB and NBODY4 compare? I. Simple models

Anders, P., Baumgardt, H., Bissantz, N. and Portegies Zwart, S. (2009) How well do STARLAB and NBODY4 compare? I. Simple models. Monthly Notices of the Royal Astronomical Society, 395 4: 2304-2316. doi:10.1111/j.1365-2966.2009.14695.x

Author Anders, P.
Baumgardt, H.
Bissantz, N.
Portegies Zwart, S.
Title How well do STARLAB and NBODY4 compare? I. Simple models
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
Publication date 2009-06
Sub-type Article (original research)
DOI 10.1111/j.1365-2966.2009.14695.x
Open Access Status DOI
Volume 395
Issue 4
Start page 2304
End page 2316
Total pages 13
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Language eng
Formatted abstract
N-body simulations are widely used to simulate the dynamical evolution of a variety of systems, among them star clusters. Much of our understanding of their evolution rests on the results of such direct N-body simulations. They provide insight in the structural evolution of star clusters, as well as into the occurrence of stellar exotica. Although the major pure N-body codes STARLAB/KIRA and NBODY4 are widely used for a range of applications, there is no thorough comparison study yet. Here, we thoroughly compare basic quantities as derived from simulations performed either with STARLAB/KIRA or NBODY4. We construct a large number of star cluster models for various stellar mass function settings (but without stellar/binary evolution, primordial binaries, external tidal fields, etc.), evolve them in parallel with STARLAB/KIRA and NBODY4, analyse them in a consistent way and compare the averaged results quantitatively. For this quantitative comparison, we develop a bootstrap algorithm for functional dependencies. We find an overall excellent agreement between the codes, both for the clusters’ structural and energy parameters as well as for the properties of the dynamically created binaries. However, we identify small differences, like in the energy conservation before core collapse and the energies of escaping stars, which deserve further studies. Our results reassure the comparability and the possibility to combine results from these two major N-body codes, at least for the purely dynamical models (i.e. without stellar/binary evolution) we performed. Further detailed comparison studies for more complex systems, e.g. including stellar/binary evolution, are required.
Keyword Methods: N-body simulations
Methods: statistical
Open clusters and associations: general
Mass black holes
Q-Index Code C1
Q-Index Status Provisional Code
Institutional Status Non-UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
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