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Thermal neutron capture cross section of the radioactive isotope Fe 60

Lederer, C; Schumann, D.; Bichler, Max; Dressler, R.; Eberhardt, K.; Endres, A.; Glorius, J.; Gobel, K; Hampel, G.; Heftrich, T; Wallner, Anton

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Background: Fifty percent of the heavy element abundances are produced via slow neutron capture reactions in different stellar scenarios. The underlying nucleosynthesis models need the input of neutron capture cross sections. Purpose: One of the fundamental signatures for active nucleosynthesis in our galaxy is the observation of long-lived radioactive isotopes, such as Fe60 with a half-life of 2.60×106 yr. To reproduce this γ activity in the universe, the nucleosynthesis of Fe60 has to be...[Show more]

dc.contributor.authorLederer, C
dc.contributor.authorSchumann, D.
dc.contributor.authorBichler, Max
dc.contributor.authorDressler, R.
dc.contributor.authorEberhardt, K.
dc.contributor.authorEndres, A.
dc.contributor.authorGlorius, J.
dc.contributor.authorGobel, K
dc.contributor.authorHampel, G.
dc.contributor.authorHeftrich, T
dc.contributor.authorWallner, Anton
dc.date.accessioned2016-06-14T23:19:05Z
dc.identifier.issn0556-2813
dc.identifier.urihttp://hdl.handle.net/1885/102744
dc.description.abstractBackground: Fifty percent of the heavy element abundances are produced via slow neutron capture reactions in different stellar scenarios. The underlying nucleosynthesis models need the input of neutron capture cross sections. Purpose: One of the fundamental signatures for active nucleosynthesis in our galaxy is the observation of long-lived radioactive isotopes, such as Fe60 with a half-life of 2.60×106 yr. To reproduce this γ activity in the universe, the nucleosynthesis of Fe60 has to be understood reliably. Methods: An Fe60 sample produced at the Paul Scherrer Institut (Villigen, Switzerland) was activated with thermal and epithermal neutrons at the research reactor at the Johannes Gutenberg-Universität Mainz (Mainz, Germany). Results: The thermal neutron capture cross section has been measured for the first time to σth=0.226(-0.049+0.044)b. An upper limit of σRI<0.50b could be determined for the resonance integral. Conclusions: An extrapolation towards the astrophysically interesting energy regime between kT=10 and 100 keV illustrates that the s-wave part of the direct capture component can be neglected.
dc.publisherAmerican Physical Society
dc.rightsAuthor/s retain copyright
dc.sourcePhysical Review C: Nuclear Physics
dc.titleThermal neutron capture cross section of the radioactive isotope Fe 60
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume92
dc.date.issued2015
local.identifier.absfor020202 - Nuclear Physics
local.identifier.ariespublicationa383154xPUB3226
local.type.statusPublished Version
local.contributor.affiliationLederer, C, University of Vienna
local.contributor.affiliationSchumann, D., Paul Scherrer Institute
local.contributor.affiliationBichler, Max, Technical University of Vienna
local.contributor.affiliationDressler, R., Paul Scherrer Institute
local.contributor.affiliationEberhardt, K., Johannes Gutenberg - University of Mainz
local.contributor.affiliationEndres, A., Goethe University
local.contributor.affiliationGlorius, J., Goethe University
local.contributor.affiliationGobel, K, Johann-Wolfgang-Goethe Universität
local.contributor.affiliationHampel, G., Johannes Gutenberg - University of Mainz
local.contributor.affiliationHeftrich, T, Johann-Wolfgang-Goethe Universität
local.contributor.affiliationWallner, Anton, College of Physical and Mathematical Sciences, ANU
local.bibliographicCitation.issue1
local.identifier.doi10.1103/PhysRevC.92.015806
dc.date.updated2016-06-14T08:32:19Z
local.identifier.scopusID2-s2.0-84938858884
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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