Show simple item record

dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorTsujimoto, T
dc.contributor.authorNomoto, K
dc.contributor.authorHachisu, I
dc.contributor.authorKato, M
dc.date.accessioned2011-12-20T15:01:07Z
dc.date.available2011-12-20T15:01:07Z
dc.date.issued1998-08-20
dc.identifier.citationKobayashi , C , Tsujimoto , T , Nomoto , K , Hachisu , I & Kato , M 1998 , ' Low-metallicity inhibition of type Ia supernovae and galactic and cosmic chemical evolution ' , Astrophysical Journal Letters , vol. 503 , no. 2 , pp. L155-L159 . https://doi.org/10.1086/311556
dc.identifier.issn2041-8213
dc.identifier.otherPURE: 494261
dc.identifier.otherPURE UUID: e4d6bc3c-5410-45c9-b1cb-f22053ec0fd8
dc.identifier.otherWOS: 000077777000013
dc.identifier.otherScopus: 22044450006
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750449
dc.identifier.urihttp://hdl.handle.net/2299/7418
dc.description.abstractWe introduce a metallicity dependence of the Type Ia supernova (SN Ia) rate into the Galactic and cosmic chemical evolution models. In our SN Ia progenitor scenario, the accreting white dwarf (WD) blows a strong wind to reach the Chandrasekhar mass limit. If the iron abundance of the progenitors is as low as [Fe/H] less than or similar to -1, then the wind is too weak for SNe Ia to occur. Our model successfully reproduces the observed chemical evolution in the solar neighborhood. We make the following predictions that can test this metallicity effect: (1) SNe Ia are not found in the low iron abundance environments such as dwarf galaxies and the outskirts of spirals. (2) 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. At z greater than or similar to 1-2, SNe Ia can be found only in the environments where the timescale of metal enrichment is sufficiently short as in starburst galaxies and elliptical galaxies. The low-metallicity inhibition of SNe Ia can shed new light on the following issues: (1) The limited metallicity range of the SN Ia progenitors would imply that "evolution effects" are relatively small for the use of high-redshift SNe Ia to determine the cosmological parameters. (2) WDs of halo populations are poor producers of SNe Ia, so that the WD contribution to the halo mass is not constrained from the iron abundance in the halo. (3) The abundance patterns of globular clusters and field stars in the Galactic halo lack of SN Ia signatures in spite of their age difference of several Gyr, which can be explained by the low-metallicity inhibition of SNe Ia. (4) It could also explain why the SN Ia contamination is not seen in the damped Ly alpha systems over a wide range of redshift.en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Letters
dc.subjectbinaries : close
dc.subjectcosmology : theory
dc.subjectgalaxies : abundances
dc.subjectgalaxies : evolution
dc.subjectGalaxy : evolution
dc.subjectsupernovae : general
dc.subjectWHITE-DWARFS
dc.subjectII SUPERNOVAE
dc.subjectHALO STARS
dc.subjectNUCLEOSYNTHESIS
dc.subjectPARAMETERS
dc.subjectOXYGEN
dc.subjectGALAXY
dc.subjectMODELS
dc.subjectDISK
dc.subjectAGES
dc.titleLow-metallicity inhibition of type Ia supernovae and galactic and cosmic chemical evolutionen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Engineering & Computer Science
dc.contributor.institutionDepartment of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1086/311556
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record