Show simple item record

dc.contributor.authorMartinez-Pinedo, G.
dc.contributor.authorMocelj, D.
dc.contributor.authorZinner, N. T.
dc.contributor.authorKelic, A.
dc.contributor.authorLanganke, K.
dc.contributor.authorPanov, I.
dc.contributor.authorPfeiffer, B.
dc.contributor.authorRauscher, T.
dc.contributor.authorSchmidt, K.-H.
dc.contributor.authorThielemann, Friedrich-Karl
dc.date.accessioned2014-12-04T09:44:38Z
dc.date.available2014-12-04T09:44:38Z
dc.date.issued2007
dc.identifier.citationMartinez-Pinedo , G , Mocelj , D , Zinner , N T , Kelic , A , Langanke , K , Panov , I , Pfeiffer , B , Rauscher , T , Schmidt , K-H & Thielemann , F-K 2007 , The role of fission in the r-process . in Progress in Particle and Nuclear Physics . Progress in Particle and Nuclear Physics , no. 1 , vol. 59 , Elsevier , pp. 199-205 , International Workshop on Nuclear Physics/28th Course Radioactive Beams, Nuclear Dynamics and Astrophysics , Erice , Italy , 16/09/06 . https://doi.org/10.1016/j.ppnp.2007.01.018
dc.identifier.citationconference
dc.identifier.issn0146-6410
dc.identifier.otherPURE: 1624416
dc.identifier.otherPURE UUID: 8dff5d80-d788-48b6-9ffc-2c6ebdabf55b
dc.identifier.otherWOS: 000248204700021
dc.identifier.otherScopus: 34248371684
dc.identifier.urihttp://hdl.handle.net/2299/14878
dc.description.abstractWe have developed a full set of fission rates that include spontaneous fission, neutron-induced fission, beta-delayed fission and, neutrino-induced fission, that are supplemented with realistic distributions of fission yields. Using this new input data we have carried out r-process calculations assuming adiabatic expansions that mimic the conditions achieved in the supernova neutrino driven wind. We have explored the sensitivity of the final abundances to different mass models. The resulting abundance distribution turns out to be very sensitive to the strength of the N = 82 shell gap far from stability. Mass models with a strong shell gap converge to an r-process distribution that is independent of the initial conditions once fission sets in. This convergence is not achieved in mass models with a quenched N = 82 shell gap. (c) 2007 Published by Elsevier B.V.en
dc.format.extent7
dc.language.isoeng
dc.publisherElsevier
dc.relation.ispartofProgress in Particle and Nuclear Physics
dc.relation.ispartofseriesProgress in Particle and Nuclear Physics
dc.subjectCHRONOMETERS
dc.subjectHEAVY ELEMENT SYNTHESIS
dc.subjectCS 31082-001
dc.subjectPROCESS NUCLEOSYNTHESIS
dc.subjectMETAL-POOR STARS
dc.subjectr-process nucleosynthesis
dc.subjectnuclei far from stability
dc.subjectMODEL
dc.subjectRICH
dc.subjectNEUTRINO-DRIVEN WINDS
dc.subjectNUCLEAR-MASS FORMULA
dc.subjectfission
dc.subjectABUNDANCES
dc.titleThe role of fission in the r-processen
dc.contributor.institutionCentre for Astrophysics Research
rioxxterms.versionofrecordhttps://doi.org/10.1016/j.ppnp.2007.01.018
rioxxterms.typeOther
herts.preservation.rarelyaccessedtrue


Files in this item

FilesSizeFormatView

There are no files associated with this item.

This item appears in the following Collection(s)

Show simple item record