Anisotropic Models of Dark Halos
arXiv:0809.3946 · doi:10.1134/S1063773708100022
Abstract
An iterative approach is used to construct spherically symmetric equilibrium models with an anisotropic velocity distribution. The potentialities of the method have been tested on models with known distribution functions, the Osipkov-Merritt models. It is shown that models that differ significantly from the Osipkov-Merritt models can be constructed. An N-body model of a dark halo with a density distribution that approximates the results of cosmological simulations (the Navarro--Frenk--White model) has been constructed. The anisotropy profile has been taken to be similar to that yielded by cosmological simulations. The constructed models can serve as direct input data for investigating the dynamics and stability of such systems in N-body simulations.
17 pages 5 figures, to be published in Astronomy Letters (v. 34, 2008)
References in corpus (21)
- A Universal Density Profile from Hierarchical Clustering
- The Structure of Cold Dark Matter Halos
- The Formation of Galactic Disks
- Cold collapse and the core catastrophe
- The Structure of Dark Matter Haloes in Hierarchical Clustering Models
- What determines the strength and the slowdown rate of bars ?
- Resolving the Structure of Cold Dark Matter Halos II
- Quantifying the Fragility of Galactic Disks in Minor Mergers
- Velocity and spatial biases in CDM subhalo distributions
- Properties of spherical galaxies and clusters with an NFW density profile
- Structure of Dark Matter Halos From Hierarchical Clustering
- Made-to-measure N-body systems
- NMAGIC: Fast Parallel Implementation of a Chi-Squared-Made-to-Measure Algorithm for Modelling Observational Data
- Velocity bias in a LCDM model
- Dynamical models with a general anisotropy profile
- Numerical stability of a family of Osipkov-Merrit models
- Velocity profiles of Osipkov-Merritt models
- Galaxy Models with Tangentially Anisotropic Velocity Distributions
- Evolution of stellar-gaseous disks in cosmological haloes
- Radial stability of a family of anisotropic Hernquist models with and without a supermassive black hole
- Phase models of the Milky Way stellar disc