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dc.contributor.authorPignatari, M.
dc.contributor.authorZinner, E.
dc.contributor.authorBertolli, M.G.
dc.contributor.authorTrappitsch, R.
dc.contributor.authorHoppe, P.
dc.contributor.authorRauscher, T.
dc.contributor.authorFryer, C.
dc.contributor.authorHerwig, F.
dc.contributor.authorHirschi, R.
dc.contributor.authorTimmes, F.X.
dc.contributor.authorThielemann, F.-K.
dc.date.accessioned2013-10-17T13:00:49Z
dc.date.available2013-10-17T13:00:49Z
dc.date.issued2013-07-01
dc.identifier.citationPignatari , M , Zinner , E , Bertolli , M G , Trappitsch , R , Hoppe , P , Rauscher , T , Fryer , C , Herwig , F , Hirschi , R , Timmes , F X & Thielemann , F-K 2013 , ' Silicon carbide grains of type C provide evidence for the production of the unstable isotope Si in supernovae ' , Astrophysical Journal Letters , vol. 771 , no. 1 , L7 . https://doi.org/10.1088/2041-8205/771/1/L7
dc.identifier.issn2041-8205
dc.identifier.otherPURE: 2061077
dc.identifier.otherPURE UUID: bad620f5-2128-42b3-a1e2-99f33d2fa9f7
dc.identifier.otherScopus: 84879953920
dc.identifier.urihttp://hdl.handle.net/2299/11809
dc.description.abstractCarbon-rich grains are observed to condense in the ejecta of recent core-collapse supernovae (SNe) within a year after the explosion. Silicon carbide grains of type X are C-rich grains with isotopic signatures of explosive SN nucleosynthesis have been found in primitive meteorites. Much rarer silicon carbide grains of type C are a special sub-group of SiC grains from SNe. They show peculiar abundance signatures for Si and S, isotopically heavy Si, and isotopically light S, which appear to be in disagreement with model predictions. We propose that C grains are formed mostly from C-rich stellar material exposed to lower SN shock temperatures than the more common type X grains. In this scenario, extreme S enrichments observed in C grains may be explained by the presence of short-lived Si (τ = 153 yr) in the ejecta, produced by neutron capture processes starting from the stable Si isotopes. No mixing from deeper Si-rich material and/or fractionation of Si from S due to molecular chemistry is needed to explain the S enrichments. The abundance of Si in the grains can provide constraints on the neutron density reached during the SN explosion in the C-rich He shell material. The impact of the large uncertainty of the neutron capture cross sections in the Si region is discussed.en
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstrophysical Journal Letters
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleSilicon carbide grains of type C provide evidence for the production of the unstable isotope Si in supernovaeen
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.versiontypeFinal Accepted Version
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1088/2041-8205/771/1/L7
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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