The impact of numerical viscosity in SPH simulations of galaxy clusters

Astronomy and Astrophysics

Volumn 526, Issue 19, 2011, Pages

  Valdarnini, R ^a  

^a SISSA   (Italy)

Author keywords

galaxies: clusters: general; methods: numerical; X rays: galaxies: clusters

Indexed keywords

AMBIENT MEDIUM; ARTIFICIAL VISCOSITY; CLUSTER CORES; CLUSTER SIMULATIONS; DISSIPATIVE EFFECTS; DYNAMICAL STATE; GALAXIES: CLUSTERS: GENERAL; GALAXY CLUSTERS; GAS PARTICLES; GAS VELOCITY; HEAT DIFFUSIONS; HYDROSTATIC EQUILIBRIUM; INNER REGION; LARGE CLUSTERS; LENGTH SCALE; LONGITUDINAL COMPONENTS; MASS CORRECTION; METHODS: NUMERICALS; NUMERICAL RESOLUTION; NUMERICAL VISCOSITY; PHYSICAL MODELING; RADIAL ENTROPY; RADIAL PROFILES; RADIATIVE LOSS; REFERENCE SOLUTION; SHOCK CONDITIONS; SPECTRAL PROPERTIES; SPH CODE; SPH SIMULATION; STATISTICAL PROPERTIES; TEST PROBLEM; THERMODYNAMIC VARIABLES; TIME EVOLUTIONS; TIME-DEPENDENT; TOTAL ENERGY; TURBULENT ENERGIES; TURBULENT HEATING; TURBULENT MOTION; VELOCITY FIELD; VISCOSITY PARAMETERS; VISCOUS DAMPING; VISCOUS DISSIPATION; WAVE NUMBERS; X RAYS: GALAXIES: CLUSTERS;

ENTROPY; GALAXIES; GASES; HIGH ENERGY PHYSICS; MODELS; NUMERICAL METHODS; POWER SPECTRUM; THERMODYNAMICS; VELOCITY; VISCOSITY; X RAYS;

MATHEMATICAL MODELS;

EID: 78651489056     PISSN: 00046361     EISSN: 14320746     Source Type: Journal    
DOI: 10.1051/0004-6361/201015340     Document Type: Article

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