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Single-particle shell strengths near the doubly magic nucleus 56Ni and the 56Ni(p,γ)57Cu reaction rate in explosive astrophysical burning

dc.contributor.authorKahl, D.
dc.contributor.authorWoods, P.J.
dc.contributor.authorPoxon-Pearson, T.
dc.contributor.authorNunes, F.M.
dc.contributor.authorBrown, B.A.
dc.contributor.authorSchatz, H.
dc.contributor.authorBaumann, T.
dc.contributor.authorBazin, D.
dc.contributor.authorBelarge, J.A.
dc.contributor.authorBender, P.C.
dc.contributor.authorElman, B.
dc.contributor.authorEstrade, A.
dc.contributor.authorGade, A.
dc.contributor.authorKankainen, A.
dc.contributor.authorLederer-Woods, C.
dc.contributor.authorLipschutz, S.
dc.contributor.authorLongfellow, B.
dc.contributor.authorLonsdale, S.-J.
dc.contributor.authorLunderberg, E.
dc.contributor.authorMontes, F.
dc.contributor.authorOng, W.J.
dc.contributor.authorPerdikakis, G.
dc.contributor.authorPereira, J.
dc.contributor.authorSullivan, C.
dc.contributor.authorTaverner, R.
dc.contributor.authorWeisshaar, D.
dc.contributor.authorZegers, R.
dc.date.accessioned2019-08-02T08:15:15Z
dc.date.available2019-08-02T08:15:15Z
dc.date.issued2019
dc.identifier.citationKahl, D., Woods, P.J., Poxon-Pearson, T., Nunes, F.M., Brown, B.A., Schatz, H., Baumann, T., Bazin, D., Belarge, J.A., Bender, P.C., Elman, B., Estrade, A., Gade, A., Kankainen, A., Lederer-Woods, C., Lipschutz, S., Longfellow, B., Lonsdale, S.-J., Lunderberg, E., . . . Zegers, R. (2019). Single-particle shell strengths near the doubly magic nucleus 56Ni and the 56Ni(p,γ)57Cu reaction rate in explosive astrophysical burning. <i>Physics Letters B</i>, <i>797</i>, Article 134803. <a href="https://doi.org/10.1016/j.physletb.2019.134803" target="_blank">https://doi.org/10.1016/j.physletb.2019.134803</a>
dc.identifier.otherCONVID_32179110
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/65191
dc.description.abstractAngle-integrated cross-section measurements of the 56Ni(d,n) and (d,p) stripping reactions have been performed to determine the single-particle strengths of low-lying excited states in the mirror nuclei pair 57Cu−57Ni situated adjacent to the doubly magic nucleus 56Ni. The reactions were studied in inverse kinematics utilizing a beam of radioactive 56Ni ions in conjunction with the GRETINA γ-array. Spectroscopic factors are compared with new shell-model calculations using a full pf model space with the GPFX1A Hamiltonian for the isospin-conserving strong interaction plus Coulomb and charge-dependent Hamiltonians. These results were used to set new constraints on the 56Ni(p,γ)57Cu reaction rate for explosive burning conditions in x-ray bursts, where 56Ni represents a key waiting point in the astrophysical rp-process.en
dc.format.mimetypeapplication/pdf
dc.languageeng
dc.language.isoeng
dc.publisherElsevier BV
dc.relation.ispartofseriesPhysics Letters B
dc.rightsCC BY 4.0
dc.subject.otherX-ray bursts
dc.subject.othershell model
dc.subject.othertransfer reactions
dc.subject.otherradioactive beams
dc.titleSingle-particle shell strengths near the doubly magic nucleus 56Ni and the 56Ni(p,γ)57Cu reaction rate in explosive astrophysical burning
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-201908023753
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.contributor.oppiaineKiihdytinlaboratoriofi
dc.contributor.oppiaineAccelerator Laboratoryen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.type.coarhttp://purl.org/coar/resource_type/c_2df8fbb1
dc.description.reviewstatuspeerReviewed
dc.relation.issn0370-2693
dc.relation.volume797
dc.type.versionpublishedVersion
dc.rights.copyright© 2019 The Author(s)
dc.rights.accesslevelopenAccessfi
dc.subject.ysoydinfysiikka
dc.format.contentfulltext
jyx.subject.urihttp://www.yso.fi/onto/yso/p14759
dc.rights.urlhttps://creativecommons.org/licenses/by/4.0/
dc.relation.doi10.1016/j.physletb.2019.134803
jyx.fundinginformationThis work was supported by the U.S. National Science Foundation (NSF) under Cooperative Agreement No. PHY-1102511 (NSCL) and No. PHY-1430152 (JINA-CEE). GRETINA was funded by the DOE, Office of Science. Operation of the array at NSCL was supported by the DOE under Grants No. DE-SC0014537 (NSCL) and No. DE-AC02-05CH11231 (LBNL). BAB kindly acknowledges funding from an NSF Grant No. PHY-1811855. The Edinburgh group is appreciative of funding from the UK STFC under Grant No. ST/L005824/1.
dc.type.okmA1


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