{"@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/1362262946023005568.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1038/ncomms6451"}},{"identifier":{"@type":"URI","@value":"https://www.nature.com/articles/ncomms6451.pdf"}},{"identifier":{"@type":"URI","@value":"https://www.nature.com/articles/ncomms6451"}}],"dc:title":[{"@value":"Pressure–temperature evolution of primordial solar system solids during impact-induced compaction"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title><jats:p>Prior to becoming chondritic meteorites, primordial solids were a poorly consolidated mix of mm-scale igneous inclusions (chondrules) and high-porosity sub-μm dust (matrix). We used high-resolution numerical simulations to track the effect of impact-induced compaction on these materials. Here we show that impact velocities as low as 1.5 km s<jats:sup>−1</jats:sup> were capable of heating the matrix to >1,000 K, with pressure–temperature varying by >10 GPa and >1,000 K over ~100 μm. Chondrules were unaffected, acting as heat-sinks: matrix temperature excursions were brief. As impact-induced compaction was a primary and ubiquitous process, our new understanding of its effects requires that key aspects of the chondrite record be re-evaluated: palaeomagnetism, petrography and variability in shock level across meteorite groups. Our data suggest a lithification mechanism for meteorites, and provide a ‘speed limit’ constraint on major compressive impacts that is inconsistent with recent models of solar system orbital architecture that require an early, rapid phase of main-belt collisional evolution.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380013168775597440","@type":"Researcher","foaf:name":[{"@value":"P. A. Bland"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005568","@type":"Researcher","foaf:name":[{"@value":"G. S. Collins"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005569","@type":"Researcher","foaf:name":[{"@value":"T. M. Davison"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005570","@type":"Researcher","foaf:name":[{"@value":"N. M. Abreu"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005572","@type":"Researcher","foaf:name":[{"@value":"F. J. Ciesla"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005574","@type":"Researcher","foaf:name":[{"@value":"A. R. Muxworthy"}]},{"@id":"https://cir.nii.ac.jp/crid/1382262946023005573","@type":"Researcher","foaf:name":[{"@value":"J. Moore"}]}],"publication":{"publicationIdentifier":[{"@type":"EISSN","@value":"20411723"}],"prism:publicationName":[{"@value":"Nature Communications"}],"dc:publisher":[{"@value":"Springer Science and Business Media LLC"}],"prism:publicationDate":"2014-12-03","prism:volume":"5","prism:number":"1","prism:startingPage":"1"},"reviewed":"false","dc:rights":["https://creativecommons.org/licenses/by/4.0","https://creativecommons.org/licenses/by/4.0"],"url":[{"@id":"https://www.nature.com/articles/ncomms6451.pdf"},{"@id":"https://www.nature.com/articles/ncomms6451"}],"createdAt":"2014-12-03","modifiedAt":"2023-01-06","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050016361176054400","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"A dehydrated space-weathered skin cloaking the hydrated interior of 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Breccias"},{"@value":"Widespread Tissintite in Strongly Shock‐Lithified Lunar Regolith Breccias"}]},{"@id":"https://cir.nii.ac.jp/crid/1050856995321851392","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Impacts may provide heat for aqueous alteration and organic solid formation on asteroid parent bodies"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004232166716288","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Mn–Cr ages and formation conditions of fayalite in CV3 carbonaceous chondrites: Constraints on the accretion ages of chondritic asteroids"}]},{"@id":"https://cir.nii.ac.jp/crid/1360021389827302144","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Structural changes in shocked tektite and their implications to impact-induced glass 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