An improved SPH scheme for cosmological simulations

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BECK, Alexander M., Giuseppe MURANTE, Alexander ARTH, Rhea-Silvia REMUS, Adelheid F. TEKLU, Julius M. F. DONNERT, Susana PLANELLES, Marcus C. BECK, Pascal FÖRSTER, Maximilian IMGRUND, Klaus DOLAG, Stefano BORGANI, 2016. An improved SPH scheme for cosmological simulations. In: Monthly Notices of the Royal Astronomical Society. 455(2), pp. 2110-2130. ISSN 0035-8711. eISSN 1365-2966. Available under: doi: 10.1093/mnras/stv2443

@article{Beck2016impro-33184, title={An improved SPH scheme for cosmological simulations}, year={2016}, doi={10.1093/mnras/stv2443}, number={2}, volume={455}, issn={0035-8711}, journal={Monthly Notices of the Royal Astronomical Society}, pages={2110--2130}, author={Beck, Alexander M. and Murante, Giuseppe and Arth, Alexander and Remus, Rhea-Silvia and Teklu, Adelheid F. and Donnert, Julius M. F. and Planelles, Susana and Beck, Marcus C. and Förster, Pascal and Imgrund, Maximilian and Dolag, Klaus and Borgani, Stefano} }

<rdf:RDF xmlns:dcterms="" xmlns:dc="" xmlns:rdf="" xmlns:bibo="" xmlns:dspace="" xmlns:foaf="" xmlns:void="" xmlns:xsd="" > <rdf:Description rdf:about=""> <dc:contributor>Donnert, Julius M. F.</dc:contributor> <dc:creator>Remus, Rhea-Silvia</dc:creator> <dc:contributor>Teklu, Adelheid F.</dc:contributor> <foaf:homepage rdf:resource="http://localhost:8080/jspui"/> <dc:contributor>Imgrund, Maximilian</dc:contributor> <dc:contributor>Remus, Rhea-Silvia</dc:contributor> <dc:creator>Beck, Alexander M.</dc:creator> <dcterms:title>An improved SPH scheme for cosmological simulations</dcterms:title> <dc:contributor>Murante, Giuseppe</dc:contributor> <dc:contributor>Dolag, Klaus</dc:contributor> <dcterms:isPartOf rdf:resource=""/> <dcterms:issued>2016</dcterms:issued> <dc:contributor>Förster, Pascal</dc:contributor> <dcterms:available rdf:datatype="">2016-03-02T09:25:43Z</dcterms:available> <dc:creator>Borgani, Stefano</dc:creator> <void:sparqlEndpoint rdf:resource="http://localhost/fuseki/dspace/sparql"/> <dc:contributor>Borgani, Stefano</dc:contributor> <dc:creator>Arth, Alexander</dc:creator> <dc:contributor>Beck, Marcus C.</dc:contributor> <dc:creator>Planelles, Susana</dc:creator> <dc:creator>Beck, Marcus C.</dc:creator> <dc:creator>Murante, Giuseppe</dc:creator> <dc:date rdf:datatype="">2016-03-02T09:25:43Z</dc:date> <dc:contributor>Arth, Alexander</dc:contributor> <dc:contributor>Planelles, Susana</dc:contributor> <dc:creator>Imgrund, Maximilian</dc:creator> <dc:creator>Förster, Pascal</dc:creator> <dcterms:abstract xml:lang="eng">We present an implementation of smoothed particle hydrodynamics (SPH) with improved accuracy for simulations of galaxies and the large-scale structure. In particular, we implement and test a vast majority of SPH improvement in the developer version of gadget-3. We use the Wendland kernel functions, a particle wake-up time-step limiting mechanism and a time-dependent scheme for artificial viscosity including high-order gradient computation and shear flow limiter. Additionally, we include a novel prescription for time-dependent artificial conduction, which corrects for gravitationally induced pressure gradients and improves the SPH performance in capturing the development of gas-dynamical instabilities. We extensively test our new implementation in a wide range of hydrodynamical standard tests including weak and strong shocks as well as shear flows, turbulent spectra, gas mixing, hydrostatic equilibria and self-gravitating gas clouds. We jointly employ all modifications; however, when necessary we study the performance of individual code modules. We approximate hydrodynamical states more accurately and with significantly less noise than standard gadget-SPH. Furthermore, the new implementation promotes the mixing of entropy between different fluid phases, also within cosmological simulations. Finally, we study the performance of the hydrodynamical solver in the context of radiative galaxy formation and non-radiative galaxy cluster formation. We find galactic discs to be colder and more extended and galaxy clusters showing entropy cores instead of steadily declining entropy profiles. In summary, we demonstrate that our improved SPH implementation overcomes most of the undesirable limitations of standard gadget-SPH, thus becoming the core of an efficient code for large cosmological simulations.</dcterms:abstract> <dc:contributor>Beck, Alexander M.</dc:contributor> <dc:creator>Dolag, Klaus</dc:creator> <dc:language>eng</dc:language> <dc:creator>Teklu, Adelheid F.</dc:creator> <dc:creator>Donnert, Julius M. F.</dc:creator> <dspace:isPartOfCollection rdf:resource=""/> <bibo:uri rdf:resource=""/> </rdf:Description> </rdf:RDF>

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