
Accession Number : ADA322030
Title : Adaptive Refinement Tree  A New HighResolution NBody Code for Cosmological Simulations,
Corporate Author : NAVAL RESEARCH LAB WASHINGTON DC SENIOR SCIENTIST FOR REACTIVE FLOW PHYSICS
Personal Author(s) : Kravtsov, Andrey V. ; Klypin, Anatoly A. ; Khokhlovq, Alexei M.
PDF Url : ADA322030
Report Date : 28 FEB 1997
Pagination or Media Count : 40
Abstract : We present a new highresolution Nbody algorithm for cosmological simulations. The algorithm employs a traditional particlemesh technique on a cubic grid and successive multilevel relaxations on the finer meshes, introduced recursively in a fully adaptive manner in the regions where the density exceeds a predefined threshold. The mesh is generated to effectively match an arbitrary geometry of the underlying density fielda property particularly important for cosmological simulations. In a simulation the mesh structure is not created at every time step but properly adjusted to the evolving particle distribution. The algorithm is fast and effectively parallel: the gravitational relaxation solver is approximately two times slower than the FFT solver on the same number of mesh cells. The required CPU time scales with number of cells, N suc c, as ^O(Nc). It allows us to improve considerably the spatial resolution of the particlemesh code without loss in mass resolution. We present a detailed description of the methodology, implementation, and tests of the code. We further use the code to study the structure of dark matter halos in highresolution (^2/h kpc) simulations of standard CDM (Omega = 1, h = 0.5, sigma sub g = 0.63) and (Lambda)CDM (0A = 1 Omega sub O = 0.7, h = 0.7, sigma sub g = 1.0) models. We find that halo density profiles in both CDM and ACDM models are well fit by the analytical model presented recently by Navarro et al. (1966) which predicts a singular (rho(r) oc 1/r) behavior of the halo density profiles at small radii. We therefore conclude that halos formed in the (Lambda)CDM model have structure similar to the CDM halos, and thus cannot explain dynamics of the central parts of dwarf spiral galaxies infrerred from their rotation curves.
Descriptors : *MATHEMATICAL MODELS, *COSMOLOGY, ALGORITHMS, SPATIAL DISTRIBUTION, RESOLUTION, MESH, SCALE, FAST FOURIER TRANSFORMS, RELAXATION, NUMERICAL METHODS AND PROCEDURES, N BODY PROBLEM.
Subject Categories : Astronomy
Distribution Statement : APPROVED FOR PUBLIC RELEASE