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dc.contributor.authorZinner, Ernst
dc.contributor.authorGöpel, Christa
dc.date.accessioned2021-02-12T20:55:40Z
dc.date.available2021-02-12T20:55:40Z
dc.date.issued2002-01-01
dc.identifier.citationZinner, E., & Göpel, C. (2002). Aluminum‐26 in H4 chondrites: Implications for its production and its usefulness as a fine‐scale chronometer for early solar system events. Meteoritics & Planetary Science, 37(7), 1001-1013.
dc.identifier.issn1945-5100
dc.identifier.doi10.1111/j.1945-5100.2002.tb00872.x
dc.identifier.urihttp://hdl.handle.net/10150/655545
dc.description.abstractIn order to investigate whether or not 26Al can be used as a fine-scale chronometer for early-solar-system events we measured, with an ion microprobe, Mg isotopes and Al/Mg ratios in separated plagioclase, olivine, and pyroxene crystals from the H4 chondrites Ste. Marguerite, Forest Vale, Beaver Creek and Quenggouk and compared the results with the canonical 26Al/27Al ratio for Ca,Al-rich inclusions (CAIs). For Ste. Marguerite (SM) and Forest Vale (FV) Pb/Pb and Mn-Cr ages have previously been determined (Gpel et al., 1994; Polnau et al., 2000; Polnau and Lugmair, 2001). Plagioclase grains from these two meteorites show clear excesses of 26Mg. The 26Al/27Al ratios inferred from these excesses and from isotopically normal Mg in pyroxene and olivine are (2.87 +/- 0.64) x 10^(-7) for SM and (1.52 +/- 0.52) x 10^(-7) for FV. The differences between these ratios and the ratio of 5 x 10^(-5) in CAIs indicate time differences of 5.4 +/- 0.1 Ma and 6.1 +/- 0.2 Ma for SM and FV, respectively. These differences are in agreement with the absolute Pb/Pb ages for CAIs and SM and FV phosphates but there are large discrepancies between the U-Pb and Mn-Cr system for the relative ages for CAIs, SM and FV. For example, Mn-Cr ages of carbonates from Kaidun are older than the Pb/Pb age of CAIs. However, even if we require that CAIs are older than these carbonates, the time difference between this "adjusted" CAI age and the Mn-Cr ages of SM and FV require that 26Al was widely distributed in the early solar system at the time of CAI formation and was not mostly present in CAIs, a feature of the X-wind model proposed by Shu and collaborators (Gounelle et al., 2001; Shu et al., 2001). From this we conclude that there was enough 26Al to melt small planetary bodies as long as they formed within 2 Ma of CAIs, and that 26Al can serve as a fine-scale chronometer for early solar system events.
dc.language.isoen
dc.publisherThe Meteoritical Society
dc.relation.urlhttps://meteoritical.org/
dc.rightsCopyright © The Meteoritical Society
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectH4 chondrites
dc.subjectMg isotopes
dc.subjectAl/Mg ratios
dc.subjectplagioclase
dc.subjectolivine
dc.subjectpyroxenes
dc.titleAluminum-26 in H4 chondrites: Implications for its production and its usefulness as a fine-scale chronometer for early solar system events
dc.typeArticle
dc.typetext
dc.identifier.journalMeteoritics & Planetary Science
dc.description.collectioninformationThe Meteoritics & Planetary Science archives are made available by the Meteoritical Society and the University of Arizona Libraries. Contact lbry-journals@email.arizona.edu for further information.
dc.eprint.versionFinal published version
dc.description.admin-noteMigrated from OJS platform February 2021
dc.source.volume37
dc.source.issue7
dc.source.beginpage1001
dc.source.endpage1013
refterms.dateFOA2021-02-12T20:55:40Z


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