dc.contributor.author | Auranen, K. | |
dc.contributor.author | Seweryniak, D. | |
dc.contributor.author | Albers, M. | |
dc.contributor.author | Ayangeakaa, A.D. | |
dc.contributor.author | Bottoni, S. | |
dc.contributor.author | Carpenter, M.P. | |
dc.contributor.author | Chiara, C.J. | |
dc.contributor.author | Copp, P. | |
dc.contributor.author | David, H.M. | |
dc.contributor.author | Doherty, D.T. | |
dc.contributor.author | Harker, J. | |
dc.contributor.author | Hoffman, C.R. | |
dc.contributor.author | Janssens, R.V.F. | |
dc.contributor.author | Khoo, T.L. | |
dc.contributor.author | Kuvin, S.A. | |
dc.contributor.author | Lauritsen, T. | |
dc.contributor.author | Lotay, G. | |
dc.contributor.author | Rogers, A.M. | |
dc.contributor.author | Scholey, Catherine | |
dc.contributor.author | Sethi, J. | |
dc.contributor.author | Talwar, R. | |
dc.contributor.author | Walters, W.B. | |
dc.contributor.author | Woods, P.J. | |
dc.contributor.author | Zhu, S. | |
dc.date.accessioned | 2019-04-18T05:53:25Z | |
dc.date.available | 2019-04-18T05:53:25Z | |
dc.date.issued | 2019 | |
dc.identifier.citation | Auranen, K., Seweryniak, D., Albers, M., Ayangeakaa, A.D., Bottoni, S., Carpenter, M.P., Chiara, C.J., Copp, P., David, H.M., Doherty, D.T., Harker, J., Hoffman, C.R., Janssens, R.V.F., Khoo, T.L., Kuvin, S.A., Lauritsen, T., Lotay, G., Rogers, A.M., 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.other | CONVID_30118603 | |
dc.identifier.other | TUTKAID_81210 | |
dc.identifier.uri | https://jyx.jyu.fi/handle/123456789/63538 | |
dc.description.abstract | Employing 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.mimetype | application/pdf | |
dc.language.iso | eng | |
dc.publisher | Elsevier BV | |
dc.relation.ispartofseries | Physics Letters B | |
dc.rights | CC BY 4.0 | |
dc.subject.other | alpha decay | |
dc.subject.other | proton decay | |
dc.subject.other | astrophysical rp process | |
dc.subject.other | 104Sb | |
dc.subject.other | 107Te | |
dc.subject.other | 108I | |
dc.title | Proton decay of 108I and its significance for the termination of the astrophysical rp-process | |
dc.type | article | |
dc.identifier.urn | URN:NBN:fi:jyu-201904152184 | |
dc.contributor.laitos | Fysiikan laitos | fi |
dc.contributor.laitos | Department of Physics | en |
dc.contributor.oppiaine | Kiihdytinlaboratorio | fi |
dc.contributor.oppiaine | Accelerator Laboratory | en |
dc.type.uri | http://purl.org/eprint/type/JournalArticle | |
dc.date.updated | 2019-04-15T15:15:06Z | |
dc.type.coar | http://purl.org/coar/resource_type/c_2df8fbb1 | |
dc.description.reviewstatus | peerReviewed | |
dc.format.pagerange | 187-192 | |
dc.relation.issn | 0370-2693 | |
dc.relation.numberinseries | 0 | |
dc.relation.volume | 792 | |
dc.type.version | publishedVersion | |
dc.rights.copyright | © 2019 Published by Elsevier B.V. | |
dc.rights.accesslevel | openAccess | fi |
dc.relation.grantnumber | 284612 | |
dc.subject.yso | astrofysiikka | |
dc.subject.yso | ydinfysiikka | |
dc.format.content | fulltext | |
jyx.subject.uri | http://www.yso.fi/onto/yso/p20188 | |
jyx.subject.uri | http://www.yso.fi/onto/yso/p14759 | |
dc.rights.url | https://creativecommons.org/licenses/by/4.0/ | |
dc.relation.doi | 10.1016/j.physletb.2019.03.039 | |
dc.relation.funder | Suomen Akatemia | fi |
dc.relation.funder | Research Council of Finland | en |
jyx.fundingprogram | Huippuyksikkörahoitus, SA | fi |
jyx.fundingprogram | Centre of Excellence, AoF | en |
jyx.fundinginformation | This 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 ). | |
dc.type.okm | A1 | |