{"@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/1361137045396767360.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1086/375856"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/592/i=2/a=1252/pdf"}},{"identifier":{"@type":"NAID","@value":"30017621233"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Evaporation of Interstellar Organic Materials in the Solar Nebula"}],"description":[{"notation":[{"@value":"A series of evaporation experiments was performed on interstellar organic analogs under high vacuum in order to study the distribution of interstellar organic materials in the solar nebula. Temperature dependences of the weight loss of the samples and the elemental composition of the evaporation residue were examined. The chemical composition of evaporated gases during heating was also investigated. It was found on the basis of the experimental results and the astrophysical model for the solar nebula that there would be molecular cloud and diffuse cloud organic materials at heliocentric distances larger than 2.7 and 2.1 AU, respectively, in the late evolution stage of the disk. Very reductive gas was evaporated at around 2.4 AU during the evaporation of diffuse cloud organic materials, and this causes very reduced condition in the solar nebula. We discuss a redox state of chondrites based on our experimental result and conclude that ordinary chondrites would form at heliocentric distances of less than 2.2 AU, enstatite chondrites at around 2.4 AU, and carbonaceous chondrites at heliocentric distances larger than 3.0 AU. From the comparison of carbon and nitrogen contents in evaporation residues of interstellar organic analogs with those in carbonaceous chondrites, it is concluded that the C and N contents in carbonaceous chondrites cannot be explained by the heating of interstellar organic dusts before accretion to parent bodies."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381137045396767361","@type":"Researcher","foaf:name":[{"@value":"Hideyuki Nakano"}]},{"@id":"https://cir.nii.ac.jp/crid/1381137045396767362","@type":"Researcher","foaf:name":[{"@value":"Akira Kouchi"}]},{"@id":"https://cir.nii.ac.jp/crid/1381137045396767360","@type":"Researcher","foaf:name":[{"@value":"Shogo Tachibana"}]},{"@id":"https://cir.nii.ac.jp/crid/1381137045396767363","@type":"Researcher","foaf:name":[{"@value":"Akira Tsuchiyama"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2003-08","prism:volume":"592","prism:number":"2","prism:startingPage":"1252","prism:endingPage":"1262"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","url":[{"@id":"http://stacks.iop.org/0004-637X/592/i=2/a=1252/pdf"}],"createdAt":"2003-07-31","modifiedAt":"2020-11-06","project":[{"@id":"https://cir.nii.ac.jp/crid/1040282256781448064","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"15340180"},{"@type":"JGN","@value":"JP15340180"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-15340180/"}],"notation":[{"@language":"ja","@value":"星間雲での光化学反応によるダイヤモンドの生成機構"},{"@language":"en","@value":"UV-induced diamond formation in interstellar clouds"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050582252660386944","@type":"Article","resourceType":"学術雑誌論文(journal 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