Evolution of Star Clusters near the Galactic Center: Fully Self-consistent N-body Simulations

Abstract

We have performed fully self-consistent $N$-body simulations of star clusters near the Galactic center (GC). Such simulations have not been performed because it is difficult to perform fast and accurate simulations of such systems using conventional methods. We used the Bridge code, which integrates the parent galaxy using the tree algorithm and the star cluster using the fourth-order Hermite scheme with individual timestep. The interaction between the parent galaxy and the star cluster is calculate with the tree algorithm. Therefore, the Bridge code can handle both the orbital and internal evolutions of star clusters correctly at the same time. We investigated the evolution of star clusters using the Bridge code and compared the results with previous studies. We found that 1) the inspiral timescale of the star clusters is shorter than that obtained with "traditional" simulations, in which the orbital evolution of star clusters is calculated analytically using the dynamical friction formula and 2) the core collapse of the star cluster increases the core density and help the cluster survive. The initial conditions of star clusters is not so severe as previously suggested.

19 pages, 19 figures, accepted for publication in ApJ

References in corpus (22)

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Cited by in corpus (22)

• The Origin of OB Runaway Stars
• In situ formation of SgrA* stars via disk fragmentation: parent cloud properties and thermodynamics
• Dynamical friction of massive objects in galactic centres
• The formation of young dense star clusters through mergers
• Dynamical constraints on the origin of the young B-stars in the Galactic center
• Constraining the initial mass function of stars in the Galactic Centre
• Growth of intermediate mass black holes by tidal disruption events in the first star clusters
• The growth of massive stars via stellar collisions in ensemble star clusters
• Trojan Stars in the Galactic Center
• The orbital motion of the Quintuplet cluster - a common origin for the Arches and Quintuplet clusters?
• The Keplerian three-body encounter I. Insights on the origin of the S-stars and the G-objects in the Galactic center
• Caught in formation: the nuclear-cluster-to-be in NGC 2139
• A Dynamical Model for Clustered Star Formation in the Galactic Disk
• Supernova Kicks and Dynamics of Compact Remnants in the Galactic Centre
• Star cluster disruption by a massive black hole binary
• Star Formation and Dynamics in the Galactic Centre
• A Scaling Relation Between Megamaser Disk Radius and Black Hole Mass in Active Galactic Nuclei
• Eccentric disc instability in stellar discs formed from inspiraling gas clouds in the Galactic Centre
• SIRIUS project II: a new tree-direct hybrid code for smoothed particle hydrodynamics/N-body simulations of star clusters
• Gravitational waves from merging intermediate-mass black holes : II Event rates at ground-based detectors
• Evolution of Star Cluster Within Galaxy using Self-consistent Hybrid Hydro/N-body Simulation
• Dynamics of star associations in an SMBH-IMBH system: The case of IRS13 in the Galactic centre