Core Collapse via Coarse Dynamic Renormalization
arXiv:astro-ph/0504546 · doi:10.1103/PhysRevLett.95.081102
Abstract
In the context of the recently developed "equation-free" approach to computer-assisted analysis of complex systems, we extract the self-similar solution describing core collapse of a stellar system from numerical experiments. The technique allows us to side-step the core "bounce" that occurs in direct N-body simulations due to the small-N correlations that develop in the late stages of collapse, and hence to follow the evolution well into the self-similar regime.
5 pages, 3 figures
References in corpus (5)
- Monte-Carlo Simulations of Globular Cluster Evolution - I. Method and Test Calculations
- The Low End of the Supermassive Black Hole Mass Function: Constraining the Mass of a Nuclear Black Hole in NGC 205 via Stellar Kinematics
- Post-Collapse evolution of globular clusters
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Cited by in corpus (13)
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- Dissipationless Formation and Evolution of the Milky Way Nuclear Star Cluster
- Performance Analysis of Direct N-Body Algorithms on Special-Purpose Supercomputers
- The Distribution of Stars and Stellar Remnants at the Galactic Center
- Gravothermal collapse of isolated self-interacting dark matter haloes: N-body simulation versus the fluid model
- Monte Carlo Simulations of Globular Cluster Evolution. IV. Direct Integration of Strong Interactions
- Dynamical Friction around Supermassive Black Holes
- Long-term evolution of massive black hole binaries. IV. Mergers of galaxies with collisionally relaxed nuclei
- Effects of Intermediate Mass Black Holes on Nuclear Star Clusters
- A new Monte Carlo method for dynamical evolution of non-spherical stellar systems
- Projective and Coarse Projective Integration for Problems with Continuous Symmetries
- Self-similar orbit-averaged Fokker-Planck equation for isotropic spherical dense clusters (i) accurate pre-collapse solution
- Self-consistent Solutions of Evolving Nuclear Star Clusters with Two-Dimensional Monte-Carlo Dynamical Simulations