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dc.contributor.authorFarouqi, K.
dc.contributor.authorKratz, K.L.
dc.contributor.authorPfeiffer, B.
dc.contributor.authorRauscher, T.
dc.contributor.authorThielemann, Friedrich-Karl
dc.contributor.authorTruran, J. W.
dc.date.accessioned2013-08-19T14:15:02Z
dc.date.available2013-08-19T14:15:02Z
dc.date.issued2010-04-01
dc.identifier.citationFarouqi , K , Kratz , K L , Pfeiffer , B , Rauscher , T , Thielemann , F-K & Truran , J W 2010 , ' Charged-particle and neutron-capture processes in the high-entropy wind of core-collapse supernovae ' , The Astrophysical Journal , vol. 712 , no. 2 , pp. 1359-1377 . https://doi.org/10.1088/0004-637X/712/2/1359
dc.identifier.issn0004-637X
dc.identifier.urihttp://hdl.handle.net/2299/11370
dc.description.abstractThe astrophysical site of the r-process is still uncertain, and a full exploration of the systematics of this process in terms of its dependence on nuclear properties from stability to the neutron drip-line within realistic stellar environments has still to be undertaken. Sufficiently high neutron-to-seed ratios can only be obtained either in very neutron-rich low-entropy environments or moderately neutron-rich high-entropy environments, related to neutron star mergers (or jets of neutron star matter) and the high-entropy wind of core-collapse supernova explosions. As chemical evolution models seem to disfavor neutron star mergers, we focus here on high-entropy environments characterized by entropy S, electron abundance Y(e), and expansion velocity V(exp). We investigate the termination point of charged-particle reactions, and we define a maximum entropy S(final) for a given V(exp) and Y(e), beyond which the seed production of heavy elements fails due to the very small matter density. We then investigate whether an r-process subsequent to the charged-particle freeze-out can in principle be understood on the basis of the classical approach, which assumes a chemical equilibrium between neutron captures and photodisintegrations, possibly followed by a beta-flow equilibrium. In particular, we illustrate how long such a chemical equilibrium approximation holds, how the freeze-out from such conditions affects the abundance pattern, and which role the late capture of neutrons originating from beta-delayed neutron emission can play. Furthermore, we analyze the impact of nuclear properties from different theoretical mass models on the final abundances after these late freeze-out phases and beta-decays back to stability. As only a superposition of astrophysical conditions can provide a good fit to the solar r-abundances, the question remains how such superpositions are attained, resulting in the apparently robust r-process pattern observed in low metallicity stars.en
dc.format.extent19
dc.format.extent1386340
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.subjectsupernovae: general
dc.subjectSTATISTICAL-MODEL CALCULATIONS
dc.subjectR-PROCESS NUCLEOSYNTHESIS
dc.subjectSun: abundances
dc.subjectII SUPERNOVAE
dc.subjectPROCESS ABUNDANCES
dc.subjectnuclear reactions, nucleosynthesis, abundances
dc.subjectASTROPHYSICAL REACTION-RATES
dc.subjectLOW-METALLICITY
dc.subjectNUCLEAR-MASS FORMULA
dc.subjectPROTONEUTRON STARS
dc.subjectDRIVEN WINDS
dc.subjectALPHA-PROCESS
dc.titleCharged-particle and neutron-capture processes in the high-entropy wind of core-collapse supernovaeen
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
rioxxterms.versionofrecord10.1088/0004-637X/712/2/1359
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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