Hydrodynamical adaptive mesh refinement simulations of turbulent flows - I. Substructure in a wind

Abstract

The problem of the resolution of turbulent flows in adaptive mesh refinement (AMR) simulations is investigated by means of 3D hydrodynamical simulations in an idealised setup, representing a moving subcluster during a merger event. AMR simulations performed with the usual refinement criteria based on local gradients of selected variables do not properly resolve the production of turbulence downstream of the cluster. Therefore we apply novel AMR criteria which are optimised to follow the evolution of a turbulent flow. We demonstrate that these criteria provide a better resolution of the flow past the subcluster, allowing us to follow the onset of the shear instability, the evolution of the turbulent wake and the subsequent back-reaction on the subcluster core morphology. We discuss some implications for the modelling of cluster cold fronts.

11 pages, 14 figures. Small changes to match the version accepted by MNRAS

References in corpus (7)

• Shocks and cold fronts in galaxy clusters
• The origin of cold fronts in the cores of relaxed galaxy clusters
• Draping of Cluster Magnetic Fields over Bullets and Bubbles -- Morphology and Dynamic Effects
• Effect of turbulent diffusion on iron abundance profiles
• Modelling Shock Heating in Cluster Mergers: I. Moving Beyond the Spherical Accretion Model
• Turbulent Velocity Fields in SPH--simulated Galaxy Clusters
• On the width of cold fronts in clusters of galaxies due to conduction

Cited by in corpus (2)

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