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dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorSpringel, Volker
dc.contributor.authorWhite, Simon D. M.
dc.date.accessioned2013-11-06T09:31:02Z
dc.date.available2013-11-06T09:31:02Z
dc.date.issued2007-04-21
dc.identifier.citationKobayashi , C , Springel , V & White , S D M 2007 , ' Simulations of cosmic chemical enrichment ' , Monthly Notices of the Royal Astronomical Society , vol. 376 , no. 4 , pp. 1465-1479 . https://doi.org/10.1111/j.1365-2966.2007.11555.x
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 811118
dc.identifier.otherPURE UUID: 41d4af23-e14f-4cd0-822f-70cecff61412
dc.identifier.otherWOS: 000245675700004
dc.identifier.otherScopus: 34247163165
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750464
dc.identifier.urihttp://hdl.handle.net/2299/11996
dc.description.abstractUsing a new numerical model for cosmic chemical evolution, we study the influence of hypernova feedback on the star formation and metal enrichment history of the universe. For assumptions which produce plausible results in idealized collapse models of individual galaxies, our cosmological simulations of the standard Lambda cold dark matter (CDM) cosmology show a peak of the cosmic star formation rate at z similar to 4, with similar to 10 per cent of the baryons turning into stars. We find that the majority of stars in present-day massive galaxies formed in much smaller galaxies at high redshifts, giving them a mean stellar age as old as 10 Gyr, despite their late assembly times. The hypernova feedback drives galactic outflows efficiently in low-mass galaxies, and these winds eject heavy elements into the intergalactic medium. The ejected baryon fraction is larger for less massive galaxies, correlates well with stellar metallicity and amounts to similar to 20 per cent of all baryons in total. The resulting enrichment history is broadly consistent with the observed abundances of Lyman break galaxies, of damped Lyman alpha systems, and of the intergalactic medium. The metallicity of the cold gas in galaxies increases with galaxy mass, which is comparable to observations with a significant scatter. The stellar mass-metallicity relation of the observed galaxy population is well reproduced by the simulation model as a result of the mass-dependent galactic winds. However, star formation does not terminate in massive galaxies at late times in our model, and too few dwarf galaxies are still forming stars. These problems may be due to a lack of resolution, to inappropriate modelling of supernova feedback or to a neglect of other feedback processes such as active galactic nuclei.en
dc.format.extent15
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsOpen
dc.subjectmethods : N-body simulations
dc.subjectgalaxies : abundances
dc.subjectgalaxies : evolution
dc.subjectgalaxies : formation
dc.subjectSTAR-FORMATION RATE
dc.subjectLYMAN-BREAK GALAXIES
dc.subjectSTELLAR MASS DENSITY
dc.subjectHUBBLE DEEP FIELD
dc.subjectHIERARCHICALLY CLUSTERING UNIVERSES
dc.subjectULTRAVIOLET LUMINOSITY DENSITY
dc.subjectSPH CHEMODYNAMICAL SIMULATION
dc.subjectCOLOR-MAGNITUDE RELATION
dc.subjectHIGH-REDSHIFT GALAXIES
dc.subjectTULLY-FISHER RELATION
dc.titleSimulations of cosmic chemical enrichmenten
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeSubmitted Version
dcterms.dateAccepted2007-04-21
rioxxterms.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1111/j.1365-2966.2007.11555.x
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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