{"@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/1363670320818864256.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1126/science.240.4860.1767"}},{"identifier":{"@type":"URI","@value":"https://www.science.org/doi/pdf/10.1126/science.240.4860.1767"}},{"identifier":{"@type":"NAID","@value":"30020535701"}}],"dc:title":[{"@value":"Deuterium on Mars: The Abundance of HDO and the Value of D/H"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>\n            Deuterium on Mars has been detected by the resolution of several Doppler-shifted lines of HDO near 3.7 micrometers in the planet's spectrum. The ratio of deuterium to hydrogen is (9 ± 4) × 10\n            <jats:sup>-4</jats:sup>\n            ; the abundance of H\n            <jats:sub>2</jats:sub>\n            0 was derived from lines near 1.1 micrometers. This ratio is enriched on Mars over the teiluric value by a factor of 6 ± 3. The enrichment implies that hydrogen escaped more rapidly from Mars in the past than it does now, consistent with a dense and warm ancient atmosphere on the planet.\n          </jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1383670320818864258","@type":"Researcher","foaf:name":[{"@value":"Tobias Owen"}],"jpcoar:affiliationName":[{"@value":"Department of Earth and Space Sciences, State University of New York, Stony Brook, NY 11794"}]},{"@id":"https://cir.nii.ac.jp/crid/1383670320818864257","@type":"Researcher","foaf:name":[{"@value":"Jean Pierre Maillard"}],"jpcoar:affiliationName":[{"@value":"Institut d'Astrophysique de Paris, F-75014 Paris, France"}]},{"@id":"https://cir.nii.ac.jp/crid/1383670320818864256","@type":"Researcher","foaf:name":[{"@value":"Catherine de Bergh"}],"jpcoar:affiliationName":[{"@value":"Observatoire de Paris, 92195 Meudon, France"}]},{"@id":"https://cir.nii.ac.jp/crid/1383670320818864259","@type":"Researcher","foaf:name":[{"@value":"Barry L. Lutz"}],"jpcoar:affiliationName":[{"@value":"Lowell Observatory, Flagstaff, AZ 86001"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00368075"},{"@type":"EISSN","@value":"10959203"}],"prism:publicationName":[{"@value":"Science"}],"dc:publisher":[{"@value":"American Association for the Advancement of Science (AAAS)"}],"prism:publicationDate":"1988-06-24","prism:volume":"240","prism:number":"4860","prism:startingPage":"1767","prism:endingPage":"1767"},"reviewed":"false","url":[{"@id":"https://www.science.org/doi/pdf/10.1126/science.240.4860.1767"}],"createdAt":"2006-10-05","modifiedAt":"2024-01-12","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050307746540945536","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"The Mars system revealed by the Martian Moons eXploration mission"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002216134712704","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Overview of the Martian atmospheric submillimetre sounder FIRE"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004232184372864","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Seasonal variation of the HDO/H2O ratio in the atmosphere of Mars at the middle of northern spring and beginning of northern summer"}]},{"@id":"https://cir.nii.ac.jp/crid/1360025429415467904","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Constraining the global composition of D/H and 18O/16O in Martian water using SOFIA/EXES"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283690892968192","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Evolution of water reservoirs on Mars: Constraints from hydrogen isotopes in martian meteorites"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283691683283456","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Hydrogen isotope evidence for loss of water from Mars through time"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285706412505344","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Water and Volatile Inventories of Mercury, Venus, the Moon, and Mars"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285707442187392","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"IR heterodyne spectrometer MILAHI for continuous monitoring observatory of Martian and Venusian atmospheres at Mt. 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