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dc.contributor.authorDemidova, S. I.
dc.contributor.authorNazarov, M. A.
dc.contributor.authorAnand, M.
dc.contributor.authorTaylor, L. A.
dc.date.accessioned2021-02-12T20:56:07Z
dc.date.available2021-02-12T20:56:07Z
dc.date.issued2003-01-01
dc.identifier.citationDemidova, S. I., Nazarov, M. A., Anand, M., & Taylor, L. A. (2003). Lunar regolith breccia Dhofar 287B: A record of lunar volcanism. Meteoritics & Planetary Science, 38(4), 501-514.
dc.identifier.issn1945-5100
dc.identifier.doi10.1111/j.1945-5100.2003.tb00023.x
dc.identifier.urihttp://hdl.handle.net/10150/655678
dc.description.abstractDhofar 287 (Dho 287), a recently found lunar meteorite, consists in large part (95%) of low-Ti mare basalt (Dho 287A) and a minor, attached portion (~5%) of regolith breccia (Dho 287B). The present study is directed mainly at the breccia portion of this meteorite. This breccia consists of a variety of lithic clasts and mineral fragments set in a fine-grained matrix and minor impact melt. The majority of clasts and minerals appear to have been mainly derived from the low-Ti basalt suite, similar to that of Dho 287A. Very low-Ti (VLT) basalts are a minor lithology of the breccia. These are significantly lower in Mg# and slightly higher in Ti compared to Luna 24 and Apollo 17 VLT basalts. Picritic glasses constitute another minor component of the breccia and are compositionally similar to Apollo 15 green glasses. Dho 287B also contains abundant fragments of Mg-rich pyroxene and anorthite-rich plagioclase grains that are absent in the lithic clasts. Such fragments appear to have been derived from a coarse-grained, Mg#-rich, Na-poor lithology. A KREEP component is apparent in chemistry, but no highlands lithologies were identified. The Dho 287 basaltic lithologies cannot be explained by near-surface fractionation of a single parental magma. Instead, magma compositions are represented by a picritic glass; a low-Ti, Na-poor glass; and a low-Ti, Na-enriched source (similar to the Dho 287A parental melt). Compositional differences among parent melts could reflect inhomogeneity of the lunar mantle. Alternatively, the low-Ti, Na-poor, and Dho 287A parent melts could be of hybrid compositions, resulting from assimilation of KREEP by picritic magma. Thus, the Dho 287B breccia contains lithologies from multiple magmatic eruptions, which differed in composition, formational conditions, and cooling histories. Based on this study, the Dho 287 is inferred to have been ejected from a region located distal to highlands terrains, possibly from the western limb of the lunar nearside, dominated by mare basalts and KREEP-rich lithologies.
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.subjectregolith breccia
dc.subjectLunar mare basalts
dc.subjectLunar petrology
dc.titleLunar regolith breccia Dhofar 287B: A record of lunar volcanism
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.volume38
dc.source.issue4
dc.source.beginpage501
dc.source.endpage514
refterms.dateFOA2021-02-12T20:56:07Z


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