Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES

TL;DR

RAMSES is a high-resolution cosmological simulation code utilizing adaptive mesh refinement, enabling detailed studies of structure formation with accurate hydrodynamics and N-body dynamics, validated through extensive tests and large-scale simulations.

Contribution

The paper introduces RAMSES, a novel AMR-based code combining N-body and hydrodynamics for cosmology, with a focus on high spatial resolution and accurate shock capturing.

Findings

Code accurately models thermal history of fluids.

Simulation results agree with analytical halo model predictions.

Numerical convergence achieved at high resolution.

Abstract

A new N-body and hydrodynamical code, called RAMSES, is presented. It has been designed to study structure formation in the universe with high spatial resolution. The code is based on Adaptive Mesh Refinement (AMR) technique, with a tree based data structure allowing recursive grid refinements on a cell-by-cell basis. The N-body solver is very similar to the one developed for the ART code (Kravtsov et al. 97), with minor differences in the exact implementation. The hydrodynamical solver is based on a second-order Godunov method, a modern shock-capturing scheme known to compute accurately the thermal history of the fluid component. The accuracy of the code is carefully estimated using various test cases, from pure gas dynamical tests to cosmological ones. The specific refinement strategy used in cosmological simulations is described, and potential spurious effects associated to shock waves propagation in the resulting AMR grid are discussed and found to be negligible. Results obtained in a large N-body and hydrodynamical simulation of structure formation in a low density LCDM universe are finally reported, with 256^3 particles and 4.1 10^7 cells in the AMR grid, reaching a formal resolution of 8192^3. A convergence analysis of different quantities, such as dark matter density power spectrum, gas pressure power spectrum and individual haloes temperature profiles, shows that numerical results are converging down to the actual resolution limit of the code, and are well reproduced by recent analytical predictions in the framework of the halo model.