Shock finding on a moving-mesh: I. Shock statistics in non-radiative cosmological simulations

  title={Shock finding on a moving-mesh: I. Shock statistics in non-radiative cosmological simulations},
  author={Kevin Schaal and Volker Springel},
  journal={Monthly Notices of the Royal Astronomical Society},
  • K. Schaal, V. Springel
  • Published 15 July 2014
  • Physics
  • Monthly Notices of the Royal Astronomical Society
Cosmological shock waves play an important role in hierarchical structure formation by dissipating and thermalizing kinetic energy of gas flows, thereby heating the universe. Furthermore, identifying shocks in hydrodynamical simulations and measuring their Mach number accurately is critical for calculating the production of non-thermal particle components through diffusive shock acceleration. However, shocks are often significantly broadened in numerical simulations, making it challenging to… 
Shock-accelerated cosmic rays and streaming instability in the adaptive mesh refinement code Ramses
Cosmic rays (CRs) are thought to play a dynamically important role in several key aspects of galaxy evolution, including the structure of the interstellar medium, the formation of galactic winds, and
Geometrical on-the-fly shock detection in smoothed particle hydrodynamics
We present an on-the-fly geometrical approach for shock detection and Mach number calculation in simulations employing smoothed particle hydrodynamics (SPH). We utilize pressure gradients to select
Simulating cosmic ray physics on a moving mesh
We discuss new methods to integrate the cosmic ray (CR) evolution equations coupled to magneto-hydrodynamics (MHD) on an unstructured moving mesh, as realised in the massively parallel AREPO code for
Exploring the role of cosmological shock waves in the Dianoga simulations of galaxy clusters
Cosmological shock waves are ubiquitous to cosmic structure formation and evolution. As a consequence, they play a major role in the energy distribution and thermalization of the intergalactic
On the interplay between cosmological shock waves and their environment
Cosmological shock waves are tracers of the thermal history of the structures in the Universe. They play a crucial role in redistributing the energy within the cosmic structures and are also amongst
SHOCKFIND - an algorithm to identify magnetohydrodynamic shock waves in turbulent clouds
The formation of stars occurs in the dense molecular cloud phase of the interstellar medium. Observations and numerical simulations of molecular clouds have shown that supersonic magnetised
On the influence of supra-thermal particle acceleration on the morphology of low-Mach, high-β shocks
When two galaxy clusters encounter each other, the interaction results in a collisionless shock that is characterized by a low (1–4) sonic Mach number, and a high-Alfvenic Mach number. Our goal is to
On the influence of supra-thermal particle acceleration on the morphology of low-Mach, high-β shocks
When two galaxy clusters encounter each other, the interaction results in a collisionless shock that is characterized by a low (1–4) sonic Mach number, and a high-Alfvénic Mach number. Our goal is
The effect of cosmic ray acceleration on supernova blast wave dynamics
Non-relativistic shocks accelerate ions to highly relativistic energies provided that the orientation of the magnetic field is closely aligned with the shock normal (quasi-parallel shock
Simulations of the dynamics of magnetized jets and cosmic rays in galaxy clusters
Feedback processes by active galactic nuclei in the centres of galaxy clusters appear to prevent large-scale cooling flows and impede star formation. However, the detailed heating mechanism remains


Detecting shock waves in cosmological smoothed particle hydrodynamics simulations
We develop a formalism for the identification and accurate estimation of the strength of structure formation shocks during cosmological smoothed particle hydrodynamics simulations. Shocks play a
Cosmological Shocks in Adaptive Mesh Refinement Simulations and the Acceleration of Cosmic Rays
We present new results characterizing cosmological shocks within adaptive mesh refinement N-body/hydrodynamic simulations that are used to predict nonthermal components of large-scale structure. This
Shock waves in Eulerian cosmological simulations: main properties and acceleration of cosmic rays
Large-scale shocks are responsible for the heating of the intracluster medium and can be important sources of cosmic rays (CRs) in the Universe. However, the occurrence and properties of these shocks
Cosmological Shock Waves in the Large-Scale Structure of the Universe: Nongravitational Effects
Cosmological shock waves result from supersonic flow motions induced by hierarchical clustering of nonlinear structures in the universe. These shocks govern the nature of cosmic plasma through
Nonlinear Particle Acceleration in Oblique Shocks
The solution of the nonlinear diffusive shock acceleration problem, where the pressure of the non-thermal population is sufficient to modify the shock hydrodynamics, is widely recognized as a key to
Modelling injection and feedback of cosmic rays in grid‐based cosmological simulations: effects on cluster outskirts
We present a numerical scheme, implemented in the cosmological adaptive mesh refinement code enzo, to model the injection of cosmic ray (CR) particles at shocks, their advection and their dynamical
Cosmological Shock Waves and Their Role in the Large-Scale Structure of the Universe
We study the properties of cosmological shock waves identified in high-resolution, N-body/hydrodynamic simulations of a ΛCDM universe and their role on thermalization of gas and acceleration of
Shocking results without shocks: Subsonic turbulence in smoothed particle hydrodynamics and moving-mesh simulations
Highly supersonic, compressible turbulence is thought to be of tantamount importance for star formation processes in the interstellar medium. Likewise, cosmic structure formation is expected to give
A comparison of cosmological codes: properties of thermal gas and shock waves in large-scale structures
Cosmological hydrodynamical simulations are a valuable tool for understanding the growth of large scale structure and the observables connected with this. Yet, comparably little attention has been
On the role of shock waves in galaxy cluster evolution
Numerical simulations of galaxy clusters including two species—baryonic gas and dark matter particles—are presented. A cold dark matter spectrum, Gaussian statistics, and flat universe are assumed.