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dc.contributor.authorEjiri, H.
dc.contributor.authorSoukouti, N.
dc.contributor.authorSuhonen, Jouni
dc.date.accessioned2016-01-25T06:41:55Z
dc.date.available2016-01-25T06:41:55Z
dc.date.issued2014
dc.identifier.citationEjiri, H., Soukouti, N., & Suhonen, J. (2014). Spin-dipole nuclear matrix elements for double beta decays and astro-neutrinos. <i>Physics Letters B</i>, <i>729</i>(February), 27-32. <a href="https://doi.org/10.1016/j.physletb.2013.12.051" target="_blank">https://doi.org/10.1016/j.physletb.2013.12.051</a>
dc.identifier.otherCONVID_23753831
dc.identifier.otherTUTKAID_62316
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/48443
dc.description.abstractSpin-dipole (SD) nuclear matrix elements (NMEs) M±(SD2) for unique first forbidden β± 2− → 0+ ground-state-to-ground-state transitions are studied by using effective microscopic two-nucleon interactions in realistic single-particle model spaces. The observed values of the NMEs M± exp(SD2) are compared with the values of the single-quasiparticle NMEs M± qp(SD2) without nucleon spin–isospin (σ τ ) correlation and the QRPA NMEs M± QRPA(SD2) with the σ τ correlation. The observed SD matrix elements are found to be reduced by the factor k ≈ 0.2 with respect to M± qp(SD2) and by the factor kNM ≈ 0.5 with respect to M± QRPA(SD2). We then infer that the SD NME is reduced considerably partly by the nucleon σ τ correlations and partly by other non-nucleonic and nucleonic correlations which are not explicitly included in the QRPA. Impact of the found reduction factors on the magnitudes of the NMEs involved in neutrino-less double beta decays and astro-neutrino interactions are discussed.
dc.language.isoeng
dc.publisherElsevier BV * North-Holland
dc.relation.ispartofseriesPhysics Letters B
dc.subject.otherspin-dipole matrix element
dc.subject.otherunique forbidden beta decay
dc.subject.otherdouble beta decay
dc.subject.otherrenormalization of the axial-vector weak
dc.subject.othercoupling constant
dc.titleSpin-dipole nuclear matrix elements for double beta decays and astro-neutrinos
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-201601201201
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.contributor.oppiaineFysiikkafi
dc.contributor.oppiainePhysicsen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.date.updated2016-01-20T13:15:23Z
dc.type.coarhttp://purl.org/coar/resource_type/c_2df8fbb1
dc.description.reviewstatuspeerReviewed
dc.format.pagerange27-32
dc.relation.issn0370-2693
dc.relation.numberinseriesFebruary
dc.relation.volume729
dc.type.versionpublishedVersion
dc.rights.copyright© 2013 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license. Funded by SCOAP3.
dc.rights.accesslevelopenAccessfi
dc.rights.urlhttp://creativecommons.org/licenses/by/3.0/
dc.relation.doi10.1016/j.physletb.2013.12.051
dc.type.okmA1


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© 2013 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license. Funded by SCOAP3.
Ellei muuten mainita, aineiston lisenssi on © 2013 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license. Funded by SCOAP3.