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dc.contributor.authorNakamura, T.
dc.contributor.authorTsuchiyama, A.
dc.contributor.authorAkaki, T.
dc.contributor.authorUesugi, K.
dc.contributor.authorNakano, T.
dc.contributor.authorTakeuchi, A.
dc.contributor.authorSuzuki, Y.
dc.contributor.authorNoguchi, T.
dc.date.accessioned2021-02-12T22:30:38Z
dc.date.available2021-02-12T22:30:38Z
dc.date.issued2008-01-01
dc.identifier.citationNakamura, T., Tsuchiyama, A., Akaki, T., Uesugi, K., Nakano, T., Takeuchi, A., ... & Noguchi, T. (2008). Bulk mineralogy and three‐dimensional structures of individual Stardust particles deduced from synchrotron X‐ray diffraction and microtomography analysis. Meteoritics & Planetary Science, 43(1‐2), 247-259.
dc.identifier.issn1945-5100
dc.identifier.doi10.1111/j.1945-5100.2008.tb00620.x
dc.identifier.urihttp://hdl.handle.net/10150/656392
dc.description.abstractDuring preliminary examination of particles released from 81P/Wild 2 short-period comet, we analyzed 28 particles by nondestructive means, high-sensitive X-ray diffraction and high-resolution X-ray tomography, in order to characterize bulk mineralogy and three-dimensional structures of individual particles. The analyses were performed at synchrotron facilities, KEK and SPring-8 in Japan. Twenty-eight particles from 5 to 25 micrometers in size, including 25 particles from Track 35 and 3 particles from Track 44, were first analyzed by X-ray diffraction and then 4 out of 28 particles were analyzed by X-ray tomography. All particles are classified into two groups based on silicate crystallinity: crystalline type and amorphous-rich type. The abundance of the former is approximately 10% of the particles investigated. Crystalline type shows very sharp reflections of olivine and low-Ca pyroxene, while amorphous-rich type shows no or very weak silicate reflections, suggesting that silicates are mostly amorphous. Broad reflections of Fe sulfides and Fe silicides are detected from most of amorphous-rich type particles. Subsequent tomography analysis revealed that the crystalline type is non-porous material consisting of coarse silicate crystals larger than 1 micrometer in size, while the amorphous-rich type is very porous aggregates with amorphous silicates and small Fe sulfide and Fe metallic grains. All characteristics of amorphousrich type particles indicate that most of them are melted and rapidly solidified during capture in the silica aerogel. On the other hand, the crystalline type is indigenous cometary particle formed through high-temperature heating episodes that have taken place prior to formation of comet Wild 2. One of the crystalline-type particles (C2054,0,35,6,0) consists of Mg-rich olivine, pyroxene, and kamacite and exhibits porphyritic or poikilitic texture very similar to chondrules.
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.subjectcometary dust
dc.subjectcosmic dust
dc.subjectx-ray diffraction
dc.subjectchemical composition of comets
dc.titleBulk mineralogy and three-dimensional structures of individual Stardust particles deduced from synchrotron X-ray diffraction and microtomography analysis
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.volume43
dc.source.issue1-2
dc.source.beginpage247
dc.source.endpage259
refterms.dateFOA2021-02-12T22:30:38Z


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