Show simple item record

dc.contributor.authorAuranen, K.
dc.contributor.authorSeweryniak, D.
dc.contributor.authorAlbers, M.
dc.contributor.authorAyangeakaa, A.D.
dc.contributor.authorBottoni, S.
dc.contributor.authorCarpenter, M.P.
dc.contributor.authorChiara, C.J.
dc.contributor.authorCopp, P.
dc.contributor.authorDavid, H.M.
dc.contributor.authorDoherty, D.T.
dc.contributor.authorHarker, J.
dc.contributor.authorHoffman, C.R.
dc.contributor.authorJanssens, R.V.F.
dc.contributor.authorKhoo, T.L.
dc.contributor.authorKuvin, S.A.
dc.contributor.authorLauritsen, T.
dc.contributor.authorLotay, G.
dc.contributor.authorRogers, A.M.
dc.contributor.authorScholey, Catherine
dc.contributor.authorSethi, J.
dc.contributor.authorTalwar, R.
dc.contributor.authorWalters, W.B.
dc.contributor.authorWoods, P.J.
dc.contributor.authorZhu, S.
dc.date.accessioned2019-04-18T05:53:25Z
dc.date.available2019-04-18T05:53:25Z
dc.date.issued2019
dc.identifier.citationAuranen, K., Seweryniak, D., Albers, M., Ayangeakaa, A., Bottoni, S., Carpenter, M., Chiara, C., Copp, P., David, H., Doherty, D., Harker, J., Hoffman, C., Janssens, R., Khoo, T., Kuvin, S., Lauritsen, T., Lotay, G., Rogers, A., Scholey, C., . . . Zhu, S. (2019). Proton decay of 108I and its significance for the termination of the astrophysical rp-process. <i>Physics Letters B</i>, <i>792</i>, 187-192. <a href="https://doi.org/10.1016/j.physletb.2019.03.039" target="_blank">https://doi.org/10.1016/j.physletb.2019.03.039</a>
dc.identifier.otherCONVID_30118603
dc.identifier.otherTUTKAID_81210
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/63538
dc.description.abstractEmploying the Argonne Fragment Mass Analyzer and the implantation-decay-decay correlation technique, a weak 0.50(21)% proton decay branch was identified in 108 I for the first time. The 108 I proton-decay width is consistent with a hindered l=2 emission, suggesting a d [Formula presented] origin. Using the extracted 108 I proton-decay Q value of 597(13) keV, and the Q α values of the 108 I and 107 Te isotopes, a proton-decay Q value of 510(20) keV for 104 Sb was deduced. Similarly to the 112,113 Cs proton-emitter pair, the Q p (I108) value is lower than that for the less-exotic neighbor 109 I, possibly due to enhanced proton-neutron interactions in N≈Z nuclei. In contrast, the present Q p (Sb104) is higher than that of 105 Sb, suggesting a weaker interaction energy. For the present Q p (Sb104) value, network calculations with the one-zone X-ray burst model Mazzocchi et al. (2007) [18] predict no significant branching into the Sn-Sb-Te cycle at 103 Sn.en
dc.format.mimetypeapplication/pdf
dc.language.isoeng
dc.publisherElsevier BV
dc.relation.ispartofseriesPhysics Letters B
dc.rightsCC BY 4.0
dc.subject.otheralpha decay
dc.subject.otherproton decay
dc.subject.otherastrophysical rp process
dc.subject.other104Sb
dc.subject.other107Te
dc.subject.other108I
dc.titleProton decay of 108I and its significance for the termination of the astrophysical rp-process
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-201904152184
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.date.updated2019-04-15T15:15:06Z
dc.description.reviewstatuspeerReviewed
dc.format.pagerange187-192
dc.relation.issn0370-2693
dc.relation.numberinseries0
dc.relation.volume792
dc.type.versionpublishedVersion
dc.rights.copyright© 2019 Published by Elsevier B.V.
dc.rights.accesslevelopenAccessfi
dc.relation.grantnumber284612
dc.subject.ysoastrofysiikka
dc.subject.ysoydinfysiikka
dc.format.contentfulltext
jyx.subject.urihttp://www.yso.fi/onto/yso/p20188
jyx.subject.urihttp://www.yso.fi/onto/yso/p14759
dc.rights.urlhttps://creativecommons.org/licenses/by/4.0/
dc.relation.doi10.1016/j.physletb.2019.03.039
dc.relation.funderSuomen Akatemiafi
dc.relation.funderAcademy of Finlanden
jyx.fundingprogramHuippuyksikkörahoitus, SAfi
jyx.fundingprogramCentre of Excellence, AoFen
jyx.fundinginformationThis material is based upon work supported by the U.S. Department of Energy, Office of Science, Office of Nuclear Physics , under Contracts No. DE-AC02-06CH11357 (ANL), No. DE-FG02-94ER40834 (UMCP), No. DE-FG02-94ER40848 (UMass Lowell), No. DE-FG02-97ER41041 (UNC), and No. DE-FG02-97ER41033 (TUNL). This research used resources of ANL's ATLAS facility, which is a DOE Office of Science User Facility. C.S. acknowledges that this work has been supported by the Academy of Finland under the Finnish Center of Excellence Programme (Contract No. 284612 ).


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record

CC BY 4.0
Except where otherwise noted, this item's license is described as CC BY 4.0