Scaling of N-body calculations

By H. Baumgardt. 2000

133 citations recorded by the source corpus.

We report results of collisional N-body simulations aimed at studying the N dependence of the dynamical evolution of star clusters. Our clusters consist of equal-mass stars and are in virial equilibrium. Clusters moving in external tidal fields and clusters limited by a cut-off radius are simulated. Our main focus is to study the dependence of the lifetimes of the clusters on the number of cluster stars and the chosen escape condition.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/0dff47de0d289ce4826b43cc5d9417873635d084

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Citations in the corpus

Globular clusters as the relics of regular star formation in ‘normal’ high-redshift galaxies (2015, methodology): “( dM dt ) evap = − M tevap , (12) on a disruption time-scale tevap = t5,evap ( M 105 M⊙ )γ , (13) where we adoptγ = 0.7 (e.g.Fukushige & Heggie 2000; Baumgardt 2001; Lamers, Gieles & Portegies Zwart 2005; Gieles & Baumgardt 2008) andt5,evap ∝ Ω−1 is the characteristic disruption time-scale of aM =…”
Disruption time scales of star clusters in different galaxies (2004, background): “Baumgardt (2001) found that for clusters in a tidal field the disruption time depends not only on the relaxation time but also on the crossing time tcr because, due to their circulation within the cluster, stars with sufficient energy still need a considerable time to reach the outskirts of the…”
Young Massive Star Clusters (2010, background): “Baumgardt (2001) showed that tdyn also enters into the escape rate and found, for equalmass stars, tdis ∝ trh3/4tdyn1/4.”
An analytical description of the disruption of star clusters in tidal fields with an application to Galactic open clusters (2005, unknown): “This dependence was found both empirically from a study of cluster samples in four galaxies by BL03 and by Lamers, Gieles & Portegies Zwart (2005), and theoretically from N -body-simulations by Baumgardt (2001) and BM03.”
Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse (2003, methodology): “For the single-component models (top curves), we include results obtained with Fokker-Planck codes (Einsel 1996; Kim et al. 2002; Quinlan 1996), Monte-Carlo codes (Joshi et al. 2001; Freitag, unpublished) and one W 0 = 3 N -body simulation by Baumgardt (2001).”
A complete N-body model of the old open cluster M67 (2005, background): “One way to reduce the mass remaining in a cluster at a certain age is to increase the strength of the tidal field in which the cluster evolves (Vesperini 1997; Baumgardt 2001).”
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS (2013, methodology): “However, more recentN-body calculations suggestα≈ 2/3 (e.g., Baumgardt 2001; Gieles & Baumgardt 2008) because of the lingering of stripped stars near the tidal radius, and we adopt this lower value for our models.”
Dynamical evolution of black hole subsystems in idealized star clusters (2013, background): “Indeed while equation 14 is a reasonable approximation, Baumgardt (2001) showed that the time scale of escape depends on both trh and the crossing time.”
Dynamical evolution of star clusters in tidal fields (2002, background): “Furthermore, as was shown by the ’Collaborative Experiment’ (Heggie et al. 1998) and Baumgardt (2001), the scaling of N-body simulations from small-N clusters up to the globular cluster regime is not without risk, especially if many processes acting on different timescales and depending on the…”
Gravitational N-Body Simulations (2003, methodology): “Simulations withNBODY 6++ forN ≤ 16K [Baumgardt, 2001] showed that the life-time does not scale with the relaxation time when the escapers are removed beyond a cutoff distance, irrespective of whether an external tidal field is present.”
The gravitational million-body problem (2001, background): “Baumgardt (2001b) shows that one consequence of this is that the initial conditions of the cluster system are more completely erased.”
An Intermediate-Mass Black Hole in the Globular Cluster G1: Improved Significance from New Keck and Hubble Space Telescope Observations (2005, background): “In fact, Baumgardt (2001) demonstrates how difficult it is to scale even simple single-mass models.”
Compact binaries in star clusters – I. Black hole binaries inside globular clusters (2009, methodology): “Tidal truncation is treated in a simplified way using the approach of Baumgardt (2001) (Giersz 2001; Giersz, Heggie & Hurley 2008).”
The life cycle of star clusters in a tidal field (2011, methodology): “This N -dependence of the escape rate is reasonably well understood, in terms of the time taken for stars to escape (Baumgardt 2001),and is included in the more refined models in Appendices A and C.”
Tidal tails of star clusters (2009, background): “The time scale of evaporation in constant tidal fields is the relaxation time, trh, as the mass loss of a tidally limited star cluster can be approximated by dM dt ∝ t −3/4 rh (1) (Baumgardt 2001).”
MODELING THE METALLICITY DISTRIBUTION OF GLOBULAR CLUSTERS (2010, background): “Baumgardt (2001) suggested that the evaporation time scales as ν−1ev ∝ t3/4rh .”