{"@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/1360004239673244416.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/aa5b8c"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/836/i=1/a=106/pdf"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/836/i=1/a=106?key=crossref.88b6a3bbfefb11e2828b7d2425dc2181"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/aa5b8c"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/aa5b8c/pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Diffusion of Oxygen Isotopes in Thermally Evolving Planetesimals and Size Ranges of Presolar Silicate Grains"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Presolar grains are small particles found in meteorites through their isotopic compositions, which are considerably different from those of materials in the solar system. If some isotopes in presolar grains diffused out beyond their grain sizes when they were embedded in parent bodies of meteorites, their isotopic compositions could be washed out, and hence the grains could no longer be identified as presolar grains. We explore this possibility for the first time by self-consistently simulating the thermal evolution of planetesimals and the diffusion length of <jats:sup>18</jats:sup>O in presolar silicate grains. Our results show that presolar silicate grains smaller than ∼0.03 <jats:italic>μ</jats:italic>m cannot keep their original isotopic compositions even if the host planetesimals experienced a maximum temperature as low as 600 °C. Since this temperature corresponds to that experienced by petrologic type 3 chondrites, isotopic diffusion can constrain the size of presolar silicate grains discovered in such chondrites to be larger than ∼0.03 <jats:italic>μ</jats:italic>m. We also find that the diffusion length of <jats:sup>18</jats:sup>O reaches ∼0.3–2 <jats:italic>μ</jats:italic>m in planetesimals that were heated up to 700–800°C. This indicates that, if the original size of presolar grains spans a range from ∼0.001 <jats:italic>μ</jats:italic>m to ∼0.3 <jats:italic>μ</jats:italic>m like that in the interstellar medium, then the isotopic records of the presolar grains may be almost completely lost in such highly thermalized parent bodies. We propose that isotopic diffusion could be a key process to control the size distribution and abundance of presolar grains in some types of chondrites.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004239673244419","@type":"Researcher","foaf:name":[{"@value":"Shigeru Wakita"}]},{"@id":"https://cir.nii.ac.jp/crid/1030003658746970115","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"90435975"},{"@type":"NRID","@value":"1000090435975"},{"@type":"NRID","@value":"9000403580144"},{"@type":"NRID","@value":"9000311497860"},{"@type":"NRID","@value":"9000403580149"},{"@type":"NRID","@value":"9000016923723"},{"@type":"NRID","@value":"9000346964646"},{"@type":"NRID","@value":"9000403580174"},{"@type":"NRID","@value":"9000239881311"},{"@type":"NRID","@value":"9000291608620"},{"@type":"NRID","@value":"9000403580135"},{"@type":"NRID","@value":"9000345347197"}],"foaf:name":[{"@value":"Takaya Nozawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673244418","@type":"Researcher","foaf:name":[{"@value":"Yasuhiro Hasegawa"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2017-02-10","prism:volume":"836","prism:number":"1","prism:startingPage":"106"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"http://stacks.iop.org/0004-637X/836/i=1/a=106/pdf"},{"@id":"http://stacks.iop.org/0004-637X/836/i=1/a=106?key=crossref.88b6a3bbfefb11e2828b7d2425dc2181"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/aa5b8c"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/aa5b8c/pdf"}],"createdAt":"2017-02-13","modifiedAt":"2024-01-10","project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257274109696","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"26400223"},{"@type":"JGN","@value":"JP26400223"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-26400223/"}],"notation":[{"@language":"ja","@value":"星周ダストをプローブとした大質量星の質量放出史と重力崩壊型超新星の多様性の解明"},{"@language":"en","@value":"Uncovering the mass-loss history of massive stars and the diversity of core-collapse supernovae through the circumstellar dust"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050306506459004160","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Effects of grain shattering by turbulence on extinction curves in starburst galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004234658434688","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Evolution of extinction curves in galaxies"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285709357472384","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FORMATION OF SiC GRAINS IN PULSATION-ENHANCED DUST-DRIVEN WIND AROUND CARBON-RICH ASYMPTOTIC GIANT BRANCH 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