{"@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/1360565166752290944.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1038/nature12163"}},{"identifier":{"@type":"URI","@value":"http://www.nature.com/articles/nature12163.pdf"}},{"identifier":{"@type":"URI","@value":"http://www.nature.com/articles/nature12163"}},{"identifier":{"@type":"PMID","@value":"23719457"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Emergence of two types of terrestrial planet on solidification of magma ocean"}],"description":[{"notation":[{"@value":"Understanding the origins of the diversity in terrestrial planets is a fundamental goal in Earth and planetary sciences. In the Solar System, Venus has a similar size and bulk composition to those of Earth, but it lacks water. Because a richer variety of exoplanets is expected to be discovered, prediction of their atmospheres and surface environments requires a general framework for planetary evolution. Here we show that terrestrial planets can be divided into two distinct types on the basis of their evolutionary history during solidification from the initially hot molten state expected from the standard formation model. Even if, apart from their orbits, they were identical just after formation, the solidified planets can have different characteristics. A type I planet, which is formed beyond a certain critical distance from the host star, solidifies within several million years. If the planet acquires water during formation, most of this water is retained and forms the earliest oceans. In contrast, on a type II planet, which is formed inside the critical distance, a magma ocean can be sustained for longer, even with a larger initial amount of water. Its duration could be as long as 100 million years if the planet is formed together with a mass of water comparable to the total inventory of the modern Earth. Hydrodynamic escape desiccates type II planets during the slow solidification process. Although Earth is categorized as type I, it is not clear which type Venus is because its orbital distance is close to the critical distance. However, because the dryness of the surface and mantle predicted for type II planets is consistent with the characteristics of Venus, it may be representative of type II planets. Also, future observations may have a chance to detect not only terrestrial exoplanets covered with water ocean but also those covered with magma ocean around a young star."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1420282801197550720","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40646171"},{"@type":"NRID","@value":"1000040646171"},{"@type":"NRID","@value":"9000239194555"},{"@type":"NRID","@value":"9000239847808"},{"@type":"NRID","@value":"9000264271319"},{"@type":"NRID","@value":"9000360597541"},{"@type":"NRID","@value":"9000283742583"}],"foaf:name":[{"@value":"Keiko Hamano"}]},{"@id":"https://cir.nii.ac.jp/crid/1380284919964434304","@type":"Researcher","foaf:name":[{"@value":"Yutaka Abe"}]},{"@id":"https://cir.nii.ac.jp/crid/1420845751167383296","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"90456260"},{"@type":"NRID","@value":"1000090456260"},{"@type":"NRID","@value":"9000252453048"},{"@type":"NRID","@value":"9000405857532"},{"@type":"NRID","@value":"9000405857533"},{"@type":"NRID","@value":"9000018860767"},{"@type":"NRID","@value":"9000314803959"},{"@type":"NRID","@value":"9000001057977"},{"@type":"NRID","@value":"9000259302872"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/genda"}],"foaf:name":[{"@value":"Hidenori Genda"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00280836"},{"@type":"EISSN","@value":"14764687"}],"prism:publicationName":[{"@value":"Nature"}],"dc:publisher":[{"@value":"Springer Science and Business Media LLC"}],"prism:publicationDate":"2013-05","prism:volume":"497","prism:number":"7451","prism:startingPage":"607","prism:endingPage":"610"},"reviewed":"false","dc:rights":["http://www.springer.com/tdm"],"url":[{"@id":"http://www.nature.com/articles/nature12163.pdf"},{"@id":"http://www.nature.com/articles/nature12163"}],"createdAt":"2013-05-28","modifiedAt":"2023-05-18","project":[{"@id":"https://cir.nii.ac.jp/crid/1040282257116812928","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"23103003"},{"@type":"JGN","@value":"JP23103003"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PLANNED-23103003/"}],"notation":[{"@language":"ja","@value":"系外惑星大気の数値モデリングと形成進化理論"},{"@language":"en","@value":"Modelling and theoretical study for exoplanet atmospheres"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282257126382592","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"23340168"},{"@type":"JGN","@value":"JP23340168"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-23340168/"}],"notation":[{"@language":"ja","@value":"衝突脱ガス水蒸気大気の分子組成と水素散逸効率の推定"},{"@language":"en","@value":"Estimation of the molecular composition and hydrogen escape rate of impact-induced steam atmospheres"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050579908119344768","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Evolution of a Water-rich Atmosphere Formed by a Giant Impact on an Earth-sized Planet"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002216061958912","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"What Hf isotopes in zircon tell us 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