{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1363388846263431040.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2006je002777"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2006JE002777"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2006JE002777"}}],"dc:title":[{"@value":"Martian Dunite NWA 2737: Petrographic constraints on geological history, shock events, and olivine color"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>Meteorite Northwest Africa (NWA) 2737 is the second known chassignite, an olivine‐rich igneous rock with mineral compositions and isotopic ratios that suggest it formed on Mars. NWA 2737 consists of ∼85% vol. olivine (Mg#, molar Mg/(Mg + Fe), of 78.3 ± 0.4%), which is notable because it is black in hand sample and brown in thin section. Other minerals include chromite, pyroxenes (augite, pigeonite, orthopyroxene), and diaplectic glass of alkali‐feldspar composition. Aqueous alteration is minimal and appears only as slight dissolution of glass. NWA 2737 formed by accumulation of olivine and chromite from a basaltic magma; the other minerals represent magma trapped among the cumulus grains. Minerals are compositionally homogeneous, consistent with chemical equilibration in late and postigneous cooling. Two‐pyroxene thermometry gives equilibration temperatures ∼1150°C, implying a significant time spent at the basalt solidus. Olivine‐spinel‐pyroxene equilibria give ∼825°C (possibly the T of mesostasis crystallization) at an oxidation state of ∼QMF‐1. This oxidation state is consistent with low Fe<jats:sup>3+</jats:sup> in olivine (determined by EMP, Mössbauer spectra, and synchrotron micro‐XANES spectroscopy) and with ∼10% of the iron in pyroxene being Fe<jats:sup>3+</jats:sup>. NWA 2737 experienced two shock events. The first shock, to stage S5–S6, affected the olivine by producing in it planar deformation features, intense mosaicism and lattice strain, and abundant droplets of iron‐nickel metal, 5–15 nm in diameter. At this stage the olivine became deeply colored, i.e., strongly absorbing at visible and near‐infrared (NIR) wavelengths. This shock event and its thermal pulse probably occurred at ∼170 Ma, the Ar‐Ar age of NWA 2737. The colored olivine is cut by ribbons of coarser, uncolored olivine with long axes along [100] and shorter axes on {021} planes: These are consistent with the easy slip law for olivine [100]{021}, which is activated at moderate strain rate at high temperature. Within these ribbons the olivine was coarsened and the iron metal globules coalesced to micron‐sized grains. The ribbons also are mosaicized and cut by planar fractures, which bespeak a second shock event, possibly that of ejection from Mars. The deeply colored olivine in NWA 2737 is unusual and represents a new “ground truth” type for remote sensing of Mars. Understanding the occurrence of the brown color in olivine in NWA 2737 places important constraints on interpretation of optical measurements.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1383388846263431168","@type":"Researcher","foaf:name":[{"@value":"Allan H. Treiman"}],"jpcoar:affiliationName":[{"@value":"Lunar and Planetary Institute  Houston Texas USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846263431040","@type":"Researcher","foaf:name":[{"@value":"M. Darby Dyar"}],"jpcoar:affiliationName":[{"@value":"Department of Astronomy Mount Holyoke College  South Hadley Massachusetts USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846263431170","@type":"Researcher","foaf:name":[{"@value":"Molly McCanta"}],"jpcoar:affiliationName":[{"@value":"Lunar and Planetary Institute  Houston Texas USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846263431041","@type":"Researcher","foaf:name":[{"@value":"Sarah K. Noble"}],"jpcoar:affiliationName":[{"@value":"ARES Division Johnson Space Center  Houston Texas USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846263431169","@type":"Researcher","foaf:name":[{"@value":"Carle M. Pieters"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Brown University  Providence Rhode Island USA"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Planets"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2007-04","prism:volume":"112","prism:number":"E4","prism:startingPage":"E04002"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2006JE002777"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2006JE002777"}],"createdAt":"2007-04-16","modifiedAt":"2023-10-12","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360567185751364352","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Mineralogical study of brown olivine in Northwest Africa 1950 shergottite and implications for the formation mechanism of iron nanoparticles"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567185751411584","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Shock veins and brown olivine in Martian meteorites: Implications for their shock pressure–temperature histories"}]},{"@id":"https://cir.nii.ac.jp/crid/1360572092879513216","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"EXAFS Determination of Clay Minerals in Martian Meteorite Allan Hills 84001 and Its Implication for the Noachian Aqueous Environment"}]},{"@id":"https://cir.nii.ac.jp/crid/1361131420707072384","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Fine‐structures of planar deformation features in shocked olivine: A comparison between Martian meteorites and experimentally shocked basalts as an indicator for shock pressure"}]},{"@id":"https://cir.nii.ac.jp/crid/1390010457712912768","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Elucidating evolution processes of Solar System bodies: Approaches by mineralogical study of various kinds of extraterrestrial materials"},{"@language":"ja","@value":"太陽系での天体進化プロセスの解明を目指して：多様な地球外物質の鉱物学的研究によるアプローチ"}]},{"@id":"https://cir.nii.ac.jp/crid/1390286981360475008","@type":"Article","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Development of Recovery Technique of Laser-Shocked Minerals: Implication to Planetary Science"},{"@language":"ja","@value":"レーザーを用いた衝撃変成手法の開発と地球惑星科学への応用"},{"@language":"ja-Kana","@value":"レーザー オ モチイタ ショウゲキ ヘンセイ シュホウ ノ カイハツ ト チキュウ ワクセイ カガク エ ノ オウヨウ"}]},{"@id":"https://cir.nii.ac.jp/crid/2050025942153536512","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Natural and experimental high-pressure, shock-produced terrestrial and extraterrestrial materials"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2006je002777"},{"@type":"CROSSREF","@value":"10.2465/gkk.220214_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.1186/s40645-021-00451-6_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.1111/maps.12949_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.1111/maps.13120_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.2184/lsj.44.9_613_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.3390/min11020176_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"},{"@type":"CROSSREF","@value":"10.1111/maps.13367_references_DOI_FAzMSECtfDxW9CAH21krQJ09L1k"}]}