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dc.contributor.authorRauscher, T.
dc.contributor.authorHeger, A.
dc.contributor.authorHoffman, R. D.
dc.contributor.authorWoosley, S.E.
dc.date.accessioned2013-06-18T09:45:43Z
dc.date.available2013-06-18T09:45:43Z
dc.date.issued2001-05-21
dc.identifier.citationRauscher , T , Heger , A , Hoffman , R D & Woosley , S E 2001 , ' Nucleosynthesis in massive stars revisited ' , Nuclear Physics A , vol. 688 , no. 1-2 , pp. 193C-196C .
dc.identifier.issn0375-9474
dc.identifier.otherPURE: 1633865
dc.identifier.otherPURE UUID: 566c65cf-40db-403f-b419-01aec6fcf15e
dc.identifier.otherWOS: 000168799300040
dc.identifier.urihttp://hdl.handle.net/2299/10811
dc.description.abstractWe have performed the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in a finely-zoned stellar model computed from the onset of central hydrogen burning through explosion as a Type II supernova. Calculations were done for 15 M-circle dot, 20 M-circle dot, and 25 M-circle dot Pop I stars using the most recently available set of experimental and theoretical nuclear data, revised opacity tables, and taking into account mass loss due to stellar winds. Here results are presented for one 15 M-circle dot model.en
dc.format.extent4
dc.language.isoeng
dc.relation.ispartofNuclear Physics A
dc.subjectR-PROCESS
dc.subjectMODEL CALCULATIONS
dc.subjectSUPERNOVAE
dc.subjectNUCLEI
dc.subjectREACTION-RATES
dc.subjectENVIRONMENTS
dc.subjectCROSS-SECTION
dc.subjectP-PROCESS
dc.titleNucleosynthesis in massive stars revisiteden
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
dcterms.dateAccepted2001-05-21
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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