E pur si muove: Galiliean-invariant cosmological hydrodynamical simulations on a moving mesh

TL;DR

This paper introduces a novel moving mesh hydrodynamics scheme for cosmological simulations that combines the advantages of Eulerian and Lagrangian methods, offering improved accuracy, Galilean invariance, and adaptive resolution.

Contribution

The paper presents a new moving mesh hydrodynamics method based on Voronoi tessellation that overcomes limitations of existing SPH and Eulerian techniques, with implementation in the AREPO code.

Findings

Achieves second-order accuracy in hydrodynamics simulations.

Maintains Galilean invariance in Lagrangian mode.

Provides automatic, continuous spatial resolution adjustment.

Abstract

Hydrodynamic cosmological simulations at present usually employ either the Lagrangian SPH technique, or Eulerian hydrodynamics on a Cartesian mesh with adaptive mesh refinement. Both of these methods have disadvantages that negatively impact their accuracy in certain situations. We here propose a novel scheme which largely eliminates these weaknesses. It is based on a moving unstructured mesh defined by the Voronoi tessellation of a set of discrete points. The mesh is used to solve the hyperbolic conservation laws of ideal hydrodynamics with a finite volume approach, based on a second-order unsplit Godunov scheme with an exact Riemann solver. The mesh-generating points can in principle be moved arbitrarily. If they are chosen to be stationary, the scheme is equivalent to an ordinary Eulerian method with second order accuracy. If they instead move with the velocity of the local flow, one obtains a Lagrangian formulation of hydrodynamics that does not suffer from the mesh distortion limitations inherent in other mesh-based Lagrangian schemes. In this mode, our new method is fully Galilean-invariant, unlike ordinary Eulerian codes, a property that is of significant importance for cosmological simulations. In addition, the new scheme can adjust its spatial resolution automatically and continuously, and hence inherits the principal advantage of SPH for simulations of cosmological structure growth. The high accuracy of Eulerian methods in the treatment of shocks is retained, while the treatment of contact discontinuities improves. We discuss how this approach is implemented in our new parallel code AREPO, both in 2D and 3D. We use a suite of test problems to examine the performance of the new code and argue that it provides an attractive and competitive alternative to current SPH and Eulerian techniques. (abridged)