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dc.contributor.authorPetermann, I.
dc.contributor.authorMartinez-Pinedo, G.
dc.contributor.authorArcones, A.
dc.contributor.authorHix, W. R.
dc.contributor.authorKelic, A.
dc.contributor.authorLanganke, K.
dc.contributor.authorPanov, I.
dc.contributor.authorRauscher, T.
dc.contributor.authorSchmidt, K-H
dc.contributor.authorThielemann, Friedrich-Karl
dc.contributor.authorZinner, N.
dc.contributor.editorFormicola, A.
dc.contributor.editorGustavino, C.
dc.contributor.editorJunker, M.
dc.date.accessioned2014-12-02T15:29:35Z
dc.date.available2014-12-02T15:29:35Z
dc.date.issued2010
dc.identifier.citationPetermann , I , Martinez-Pinedo , G , Arcones , A , Hix , W R , Kelic , A , Langanke , K , Panov , I , Rauscher , T , Schmidt , K-H , Thielemann , F-K & Zinner , N 2010 , Network calculations for r-process nucleosynthesis . in A Formicola , C Gustavino & M Junker (eds) , Nuclear Physics in Astrophysics (NPAIV 2009) . , 012008 , Journal of Physics Conference Series , no. 1 , vol. 202 , IOP PUBLISHING LTD , Bristol , 4th International Conference on Nuclear Physics in Astrophysics , Frascati , Italy , 8/06/09 . https://doi.org/10.1088/1742-6596/202/1/012008
dc.identifier.citationconference
dc.identifier.issn1742-6588
dc.identifier.otherPURE: 1619634
dc.identifier.otherPURE UUID: b6490aac-8160-4784-8987-6bec5b834843
dc.identifier.otherWOS: 000287821100008
dc.identifier.otherScopus: 77950498520
dc.identifier.urihttp://hdl.handle.net/2299/14853
dc.description.abstractThe r-process is known to be responsible for the synthesis of about half of the elements heavier than iron, nevertheless its astrophysical site has not yet been clearly ascertained, but observations indicate that at least two possible sites should contribute to the solar system abundance oft-process elements. The r-process being responsible for the production of elements heavier than Z = 56 operates rather robustly always resulting in a similar relative abundance pattern. From the nuclear-physics point of view the r-process requires the knowledge of a large number of reaction rates involving exotic nuclei that are not accessible by experiment and data have to be provided by theoretical predictions. We have developed for the first time a complete database of reaction rates that in addition to neutron-capture rates and beta-decay half-lives includes the dominant reactions that can induce fission (neutron-capture, beta-decay and spontaneous fission) and the corresponding fission yields. In addition, we have implemented these reaction rates in a fully implicit reaction network. The influence of the nuclear physics input constituted in the reaction rates based on the two mass models FRDM and ETFSI and on the astrophysical conditions simulating a cold or hot environment are examined.en
dc.format.extent4
dc.language.isoeng
dc.publisherIOP PUBLISHING LTD
dc.relation.ispartofNuclear Physics in Astrophysics (NPAIV 2009)
dc.relation.ispartofseriesJournal of Physics Conference Series
dc.subjectFISSION
dc.titleNetwork calculations for r-process nucleosynthesisen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionScience & Technology Research Institute
dc.contributor.institutionCentre for Astrophysics Research
rioxxterms.versionofrecordhttps://doi.org/10.1088/1742-6596/202/1/012008
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue


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