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dc.contributor.authorRauscher, T.
dc.contributor.authorHeger, A.
dc.contributor.authorHoffman, R. D.
dc.contributor.authorWoosley, S.E.
dc.date.accessioned2013-05-07T12:55:01Z
dc.date.available2013-05-07T12:55:01Z
dc.date.issued2002-09-01
dc.identifier.citationRauscher , T , Heger , A , Hoffman , R D & Woosley , S E 2002 , ' Nucleosynthesis in massive stars with improved nuclear and stellar physics ' , The Astrophysical Journal , vol. 576 , no. 1 , pp. 323-348 . https://doi.org/10.1086/341728
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 1632878
dc.identifier.otherPURE UUID: 6eaf623b-3cc0-4452-9a21-c697abbd99e1
dc.identifier.otherWOS: 000177589100029
dc.identifier.otherScopus: 0000814894
dc.identifier.urihttp://hdl.handle.net/2299/10634
dc.description.abstractWe present the first calculations to follow the evolution of all stable nuclei and their radioactive progenitors in stellar models computed from the onset of central hydrogen burning through explosion as Type II supernovae. Calculations are performed for Population I stars of 15, 19, 20, 21, and 25 M-circle dot using the most recently available experimental and theoretical nuclear data, revised opacity tables, neutrino losses, and weak interaction rates and taking into account mass loss due to stellar winds. A novel "adaptive" reaction network is employed with a variable number of nuclei ( adjusted each time step) ranging from similar to700 on the main sequence to greater than or similar to2200 during the explosion. The network includes, at any given time, all relevant isotopes from hydrogen through polonium (Z = 84). Even the limited grid of stellar masses studied suggests that overall good agreement can be achieved with the solar abundances of nuclei between O-16 and Zr-90. Interesting discrepancies are seen in the 20 M-circle dot model and ( so far, only in that model) are a consequence of the merging of the oxygen, neon, and carbon shells about a day prior to core collapse. We find that, in some stars, most of the "p-process" nuclei can be produced in the convective oxygen-burning shell moments prior to collapse; in others, they are made only in the explosion. Serious deficiencies still exist in all cases for the p-process isotopes of Ru and Mo.en
dc.format.extent26
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsOpen
dc.subjectC-12(ALPHA,GAMMA)O-16 REACTION-RATE
dc.subjectTHERMONUCLEAR REACTION-RATES
dc.subjectSTATISTICAL-MODEL CALCULATIONS
dc.subjectsupernovae : general
dc.subjectWEAK-INTERACTION RATES
dc.subjectR-PROCESS
dc.subjectnuclear reactions, nucleosynthesis, abundances stars : evolution
dc.subjectCROSS-SECTIONS
dc.subjectM-CIRCLE-DOT
dc.subjectASTROPHYSICAL REACTION-RATES
dc.subjectCORE-COLLAPSE SUPERNOVAE
dc.subjectP-PROCESS
dc.titleNucleosynthesis in massive stars with improved nuclear and stellar physicsen
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
dcterms.dateAccepted2002-09-01
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.1086/341728
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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