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arxiv: 1012.1885 · v1 · submitted 2010-12-08 · 🌌 astro-ph.IM · astro-ph.CO· astro-ph.SR· physics.flu-dyn· physics.plasm-ph

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Smoothed Particle Hydrodynamics and Magnetohydrodynamics

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classification 🌌 astro-ph.IM astro-ph.COastro-ph.SRphysics.flu-dynphysics.plasm-ph
keywords giveparticlebasiccodeequationshydrodynamicsinstabilitiesmagnetohydrodynamics
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This paper presents an overview and introduction to Smoothed Particle Hydrodynamics and Magnetohydrodynamics in theory and in practice. Firstly, we give a basic grounding in the fundamentals of SPH, showing how the equations of motion and energy can be self-consistently derived from the density estimate. We then show how to interpret these equations using the basic SPH interpolation formulae and highlight the subtle difference in approach between SPH and other particle methods. In doing so, we also critique several `urban myths' regarding SPH, in particular the idea that one can simply increase the `neighbour number' more slowly than the total number of particles in order to obtain convergence. We also discuss the origin of numerical instabilities such as the pairing and tensile instabilities. Finally, we give practical advice on how to resolve three of the main issues with SPMHD: removing the tensile instability, formulating dissipative terms for MHD shocks and enforcing the divergence constraint on the particles, and we give the current status of developments in this area. Accompanying the paper is the first public release of the NDSPMHD SPH code, a 1, 2 and 3 dimensional code designed as a testbed for SPH/SPMHD algorithms that can be used to test many of the ideas and used to run all of the numerical examples contained in the paper.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics

    astro-ph.CO 2026-05 unverdicted novelty 6.0

    FLAMINGO simulations show tSZ cross-correlations scale as S8 to the power of about 3 and favor low S8=0.72 with strong feedback when compared to SDSS, BOSS, DES, and Planck data.

  2. FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics

    astro-ph.CO 2026-05 conditional novelty 6.0

    tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.