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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.
Except where otherwise noted, this item's license is described as © 2013 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license. Funded by SCOAP3.