An SPH code for galaxy formation problems; Presentation of the code

Simple item page
dc.creatorHultman, John
dc.creatorKaellander, Daniel
dc.date1997-11-12
dc.date.accessioned2026-07-07T02:25:03Z
dc.date.available2026-07-07T02:25:03Z
dc.descriptionWe present and test a code for two-fluid simulations of galaxy formation, one of the fluids being collision-less. The hydrodynamical evolution is solved through the SPH method while gravitational forces are calculated using a tree method. The code is Lagrangian, and fully adaptive both in space and time. A significant fraction gas in simulations of hierarchical galaxy formation ends up in tight clumps where it is, in terms of computational effort, very expensive to integrate the SPH equations. Furthermore, this is a computational waste since these tight gas clumps are typically not gravitationally resolved. We solve this by merging gas particles in these regions, thereby limiting the SPH resolution to the gravitational force resolution, and further speeding up the simulation through the reduction in the number of particles.
dc.description15 pages, 16 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/9711136
dc.identifierhttp://arxiv.org/abs/astro-ph/9711136
dc.identifierAstron.Astrophys. 324 (1997) 534-548
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/11788
dc.subjectAstrophysics
dc.titleAn SPH code for galaxy formation problems; Presentation of the code
dc.typetext

Files

Collections

arXiv