Inviscid SPH

Abstract

In smooth-particle hydrodynamics (SPH), artificial viscosity is necessary for the correct treatment of shocks, but often generates unwanted dissipation away from shocks. We present a novel method of controlling the amount of artificial viscosity, which uses the total time derivative of the velocity divergence as shock indicator and aims at completely eliminating viscosity away from shocks. We subject the new scheme to numerous tests and find that the method works at least as well as any previous technique in the strong-shock regime, but becomes virtually inviscid away from shocks, while still maintaining particle order. In particular sound waves or oscillations of gas spheres are hardly damped over many periods.

14 pages (15 in arXiv), 15 figures, accepted for publication in MNRAS

References in corpus (8)

• The cosmological simulation code GADGET-2
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Cosmological SPH simulations: The entropy equation
• Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH
• Turbulent gas motions in galaxy cluster simulations: The role of SPH viscosity
• A Hierarchical O(N) Force Calculation Algorithm
• VINE -- A numerical code for simulating astrophysical systems using particles I: Description of the physics and the numerical methods
• SPH Simulations of Accretion Disks and Narrow Rings

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