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dc.contributor.authorHeger, A.
dc.contributor.authorWoosley, S.E.
dc.contributor.authorRauscher, T.
dc.contributor.authorHoffman, R. D.
dc.contributor.authorBoyes, M.M.
dc.date.accessioned2013-05-07T13:25:00Z
dc.date.available2013-05-07T13:25:00Z
dc.date.issued2002-07
dc.identifier.citationHeger , A , Woosley , S E , Rauscher , T , Hoffman , R D & Boyes , M M 2002 , ' Massive star evolution : nucleosynthesis and nuclear reaction rate uncertainties ' , New Astronomy Reviews , vol. 46 , no. 8-10 , pp. 463-468 . https://doi.org/10.1016/S1387-6473(02)00184-7
dc.identifier.issn1387-6473
dc.identifier.otherPURE: 1633067
dc.identifier.otherPURE UUID: 56794a90-4367-47d8-9540-06f9fd51b2e6
dc.identifier.otherWOS: 000177372400003
dc.identifier.otherScopus: 0036068941
dc.identifier.urihttp://hdl.handle.net/2299/10641
dc.description.abstractWe present a nucleosynthesis calculation of a 25 M-circle dot star of solar composition that includes all relevant isotopes up to polonium. We follow the stellar evolution from hydrogen burning till iron core collapse and simulate the explosion using a 'piston' approach. We discuss the influence of two key nuclear reaction rates, C-12(alpha, gamma)O-16 and Ne-22(alpha, n)Mg-25, on stellar evolution and nucleosynthesis. The former significantly influences the resulting core sizes (iron, silicon, oxygen) and the overall presupernova structure of the star. It thus has significant consequences for the supernova explosion itself and the compact remnant formed. The later rate considerably affects the s-process in massive stars and we demonstrate the changes that different currently suggested values for this rate cause. (C) 2002 Elsevier Science B.V. All rights reserved.en
dc.format.extent6
dc.language.isoeng
dc.relation.ispartofNew Astronomy Reviews
dc.subjectStars : massive, evolution, nucleosynthesis
dc.subjectNuclear physics : uncertainties
dc.titleMassive star evolution : nucleosynthesis and nuclear reaction rate uncertaintiesen
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.versionSMUR
rioxxterms.versionofrecordhttps://doi.org/10.1016/S1387-6473(02)00184-7
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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