Numerical Convergence of Hydrodynamical SPH Simulations of Cooling Clusters

Simple item page
dc.creatorValdarnini, R.
dc.date2001-11-05
dc.date.accessioned2026-07-07T02:01:12Z
dc.date.available2026-07-07T02:01:12Z
dc.descriptionThe results from hydrodynamical TREESPH simulations of galaxy clusters are used to investigate the dependence of the final cluster X-ray properties upon the numerical resolution and the assumed star formation models for the cooled gas. A comparison between runs with different star formation methods shows that the results of simulations, based on star formation methods in which gas conversion into stars is controlled by an efficiency parameter c_{star}, are sensitive to the simulation numerical resolution. In this respect star formation methods based instead on a local density threshold, are shown to give more stable results. Final X-ray luminosities are found to be numerically stable, with uncertainties of a factor 2.
dc.description7 pages, 2 figures, to appear in "Chemical enrichment of the intracluster and intergalactic medium", Vulcano 2001, ASP Conference Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0111076
dc.identifierhttp://arxiv.org/abs/astro-ph/0111076
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3663
dc.subjectAstrophysics
dc.titleNumerical Convergence of Hydrodynamical SPH Simulations of Cooling Clusters
dc.typetext

Files

Collections

arXiv