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dc.contributor.authorNomoto, K
dc.contributor.authorNakamura, T
dc.contributor.authorKobayashi, Chiaki
dc.date.accessioned2011-12-20T15:01:09Z
dc.date.available2011-12-20T15:01:09Z
dc.date.issued1999
dc.identifier.citationNomoto , K , Nakamura , T & Kobayashi , C 1999 , ' Supernova nucleosynthesis, chemical evolution, and cosmic supernova rate ' , Astrophysics and Space Science , vol. 265 , no. 1-4 , pp. 37-47 . https://doi.org/10.1023/A:1002136016979
dc.identifier.issn0004-640X
dc.identifier.otherPURE: 494611
dc.identifier.otherPURE UUID: 9d0b9edc-d392-4775-a32a-a508720ee7af
dc.identifier.otherWOS: 000086718900007
dc.identifier.otherScopus: 0346073574
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750423
dc.identifier.urihttp://hdl.handle.net/2299/7419
dc.description.abstractIn the chemical evolution of the Galaxy, Type II supernovae (SNe II) have contributed to the early metal enrichment and later Type Ia supernovae (SNe Ia) have contributed to the delayed enrichment of Fe. In principle, hypothetical pre-galactic population III objects could cause the earliest heavy element enrichment. Here we present our two new findings. 1) The peculiar abundance pattern among iron peak elements (Cr, Mn, Co, and Fe) in the very metal poor can be reproduced with SN II nucleosynthesis yields without invoking the contribution from Pop III objects. 2) The observed chemical evolution in the solar neighborhood is well reproduced with the metallicity dependent occurrence of SNe Ia, where SNe Ia do not occur if the iron abundance of the progenitors is as low as [Fe/H] less than or similar to 1. We make the prediction that the cosmic SN Ia rate drops at z similar to 1 - 2 because of the low-iron abundance, which can be observed with the Next Generation Space Telescope.en
dc.format.extent11
dc.language.isoeng
dc.relation.ispartofAstrophysics and Space Science
dc.subjectIA SUPERNOVAE
dc.subjectABUNDANCE RATIOS
dc.subjectMETALLICITY
dc.subjectGALAXIES
dc.subjectORIGIN
dc.subjectMODEL
dc.subjectSTARS
dc.titleSupernova nucleosynthesis, chemical evolution, and cosmic supernova rateen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1023/A:1002136016979
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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