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Convergence of SPH and AMR simulations

Published online by Cambridge University Press:  27 April 2011

David A. Hubber ,
Sam A. E. G. Falle  and
Simon P. Goodwin
David A. Hubber
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
Sam A. E. G. Falle
Affiliation:
Department of Applied Mathematics, University of Leeds, Leeds, LS2 9JT, UK
Simon P. Goodwin
Affiliation:
Department of Physics and Astronomy, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK
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Abstract

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We present the first results of a large suite of convergence tests between Adaptive Mesh Refinement (AMR) Finite Difference Hydrodynamics and Smoothed Particle Hydrodynamics (SPH) simulations of the non-linear thin shell instability and the Kelvin-Helmholtz instability. We find that the two methods converge in the limit of high resolution and accuracy. AMR and SPH simulations of the non-linear thin shell instability converge with each other with standard algorithms and parameters. The Kelvin-Helmholtz instability in SPH requires both an artificial conductivity term and a kernel with larger compact support and more neighbours (e.g. the quintic kernel) in order converge with AMR. For purely hydrodynamical problems, SPH simulations take an order of magnitude longer than the grid code when converged.

Keywords

hydrodynamicsmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 429 - 432
Copyright
Copyright © International Astronomical Union 2011

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