Show simple item record

dc.contributor.authorKobayashi, C.
dc.date.accessioned2013-12-19T14:30:19Z
dc.date.available2013-12-19T14:30:19Z
dc.date.issued2005-08-21
dc.identifier.citationKobayashi , C 2005 , ' GRAPE-SPH chemodynamical simulation of elliptical galaxies - II : Scaling relations and the fundamental plane ' , Monthly Notices of the Royal Astronomical Society , vol. 361 , no. 4 , pp. 1216-1226 . https://doi.org/10.1111/j.1365-2966.2005.09258.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 811185
dc.identifier.otherPURE UUID: 431ddf58-33e8-4137-aac0-47c1b3c6f859
dc.identifier.otherWOS: 000231459500012
dc.identifier.otherScopus: 23944519381
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750458
dc.identifier.urihttp://hdl.handle.net/2299/12439
dc.description.abstractWe simulate the formation and chemodynamical evolution of 128 elliptical galaxies using a GRAPE-SPH code that includes various physical processes that are associated with the fort-nation of stellar systems: radiative cooling, star formation, feedback from Type 11 and la supernovae and stellar winds, and chemical enrichment. We find that the star formation time-scale controls when and where stars form in the contracting gas cloud, determines the effective radius at given mass, and is constrained by observation to be 10 times longer than the local dynamical time-scale. We succeed in reproducing the observed global scaling relations under our cold dark matter based scenario, e.g. the Faber-Jackson relation, the Kormendy relation and the fundamental plane. An intrinsic scatter exists along the fundamental plane, and the origin of this scatter lies in differences in merging history. Galaxies that undergo major merger events tend to have larger effective radii and fainter surface brightnesses, which result in larger masses, smaller surface brightnesses and larger mass-to-light ratios. We can also reproduce the observed colour-magnitude and mass-metallicity relations, although the scatter is larger than observed. The scatter arises because feedback is not very effective and star formation does not terminate completely in our simulations. similar to 25 per cent of accreted baryons are blown away in the simulations, independent of the assumed star formation time-scale and initial mass function. Most heavy elements end up locked into stars in the galaxy. The ejected metal fraction depends only on the star formation time-scale, and is similar to 2 per cent even to rapid star formation.en
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectmethods : N-body simulations
dc.subjectgalaxies : abundances
dc.subjectgalaxies : elliptical and lenticular, cD
dc.subjectgalaxies : evolution
dc.subjectgalaxies : formation
dc.subjectDYNAMICALLY HOT GALAXIES
dc.subjectCOLOR-MAGNITUDE RELATION
dc.subjectGROTH STRIP SURVEY
dc.subjectDISTANT CLUSTERS
dc.subjectFIELD GALAXIES
dc.subjectSTELLAR POPULATIONS
dc.subjectSAURON PROJECT
dc.subjectSTAR-FORMATION
dc.subjectEVOLUTION
dc.subjectPHOTOMETRY
dc.titleGRAPE-SPH chemodynamical simulation of elliptical galaxies - II : Scaling relations and the fundamental planeen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
dcterms.dateAccepted2005-08-21
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2005.09258.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record