Näytä suppeat kuvailutiedot

dc.contributor.authorMargerin, V.
dc.contributor.authorMurphy, A.St.J.
dc.contributor.authorDavinson, T.
dc.contributor.authorDressler, R.
dc.contributor.authorFallis, J.
dc.contributor.authorKankainen, Anu
dc.contributor.authorLaird, A.M.
dc.contributor.authorLotay, G.
dc.contributor.authorMountford, D.J.
dc.contributor.authorMurphy, C.D.
dc.contributor.authorSeiffert, C.
dc.contributor.authorSchumann, D.
dc.contributor.authorStowasser, T.
dc.contributor.authorStora, T.
dc.contributor.authorWang, C.H.-T.
dc.contributor.authorWoods, P.J.
dc.date.accessioned2016-02-03T10:41:06Z
dc.date.available2016-02-03T10:41:06Z
dc.date.issued2014
dc.identifier.citationMargerin, V., Murphy, A.St.J., Davinson, T., Dressler, R., Fallis, J., Kankainen, A., Laird, A.M., Lotay, G., Mountford, D.J., Murphy, C.D., Seiffert, C., Schumann, D., Stowasser, T., Stora, T., Wang, C.H.-T., & Woods, P.J. (2014). Study of the Ti-44(alpha, p)V-47 reaction and implications for core collapse supernovae. <i>Physics Letters B</i>, <i>731</i>(April), 358-361. <a href="https://doi.org/10.1016/j.physletb.2014.03.003" target="_blank">https://doi.org/10.1016/j.physletb.2014.03.003</a>
dc.identifier.otherCONVID_23727324
dc.identifier.otherTUTKAID_62162
dc.identifier.urihttps://jyx.jyu.fi/handle/123456789/48588
dc.description.abstractThe underlying physics triggering core collapse supernovae is not fully understood but observations of material ejected during such events helps to solve this puzzle. In particular, several satellite based γ -ray observations of the isotope 44Ti have been reported recently. Conveniently, the amount of this isotope in stellar ejecta is thought to depend critically on the explosion mechanism. The most influential reaction to the amount of 44Ti in supernovae is 44Ti(α, p)47V. Here we report on a direct study of this reaction conducted at the REX-ISOLDE facility, CERN. The experiment was performed with a 44Ti beam at Elab = 2.16 MeV/u, corresponding to an energy distribution, for reacting α-particles, centred on Ecm = 4.15 with a 1σ width of 0.23 MeV. This is, for the first time, well within the Gamow window for core collapse supernovae. The material from which the 44Ti beam was extracted originates from highly irradiated components of the SINQ spallation neutron source of the Paul Scherrer Institute. No yield above background was observed, enabling an upper limit for the rate of this reaction to be determined. This result is below expectation, suggesting that the 44Ti(α, p)47V reaction proceeds more slowly than previously thought. Implications for astrophysical events, and remnant age, are discussed.
dc.language.isoeng
dc.publisherElsevier BV * North-Holland
dc.relation.ispartofseriesPhysics Letters B
dc.subject.otherstatistical-model calculations
dc.subject.otherastrophysical reaction-rates
dc.subject.otheracceretion shock
dc.subject.otherTI-44
dc.subject.other1987A
dc.subject.otheremission
dc.subject.otherinstability
dc.subject.othercassiopeia
dc.subject.othertarget
dc.titleStudy of the Ti-44(alpha, p)V-47 reaction and implications for core collapse supernovae
dc.typearticle
dc.identifier.urnURN:NBN:fi:jyu-201602021379
dc.contributor.laitosFysiikan laitosfi
dc.contributor.laitosDepartment of Physicsen
dc.contributor.oppiaineFysiikkafi
dc.contributor.oppiaineKiihdytinlaboratoriofi
dc.contributor.oppiainePhysicsen
dc.contributor.oppiaineAccelerator Laboratoryen
dc.type.urihttp://purl.org/eprint/type/JournalArticle
dc.date.updated2016-02-02T10:15:05Z
dc.type.coarhttp://purl.org/coar/resource_type/c_2df8fbb1
dc.description.reviewstatuspeerReviewed
dc.format.pagerange358-361
dc.relation.issn0370-2693
dc.relation.numberinseriesApril
dc.relation.volume731
dc.type.versionpublishedVersion
dc.rights.copyright© 2014 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.subject.ysoherkkyys (psykologia)
jyx.subject.urihttp://www.yso.fi/onto/yso/p20121
dc.rights.urlhttp://creativecommons.org/licenses/by/3.0/
dc.relation.doi10.1016/j.physletb.2014.03.003
dc.type.okmA1


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Näytä suppeat kuvailutiedot

© 2014 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 © 2014 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY license. Funded by SCOAP3.