{"@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/1360286991877815552.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1016/j.icarus.2019.113567"}},{"identifier":{"@type":"URI","@value":"https://api.elsevier.com/content/article/PII:S0019103518300927?httpAccept=text/xml"}},{"identifier":{"@type":"URI","@value":"https://api.elsevier.com/content/article/PII:S0019103518300927?httpAccept=text/plain"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"A coupled atmosphere–hydrosphere global climate model of early Mars: A ‘cool and wet’ scenario for the formation of water channels"}],"description":[{"notation":[{"@value":"Abstract   Martian water channels are considered evidence of a climate warm enough to allow the existence of long-term fluvial systems on early Mars during the Noachian and Hesperian boundary (3.85–3.6 Ga). Quantitative inferences of water channel formation from climate models are crucial to develop an accurate understanding of the early Martian environment. We present the results of a newly developed 3-dimensional Paleo Martian Global Climate Model (PMGCM) assuming a CO2/H2O/H2 atmosphere under the ‘Faint Young Sun’ condition (with a solar luminosity of ~75% of the current value) for surface pressures between 0.5 and 2 bar. The PMGCM has a hydrologic cycle module, which includes ocean thermodynamics and water vapor advection, convection, condensation and precipitation processes, as well as calculations of surface fluvial activities (e.g., fluvial activity and sediment transport) at a high horizontal resolution.  Our PMGCM results show that the early Martian surface environment could have been ‘cool’ (between ‘warm’ and ‘cold’); namely, the surface temperatures could have been high enough (>273 K) during summertime to allow seasonal melting of snow and ice deposits, and low enough ("}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380021391873340699","@type":"Researcher","foaf:name":[{"@value":"A. Kamada"}]},{"@id":"https://cir.nii.ac.jp/crid/1380286991877815556","@type":"Researcher","foaf:name":[{"@value":"T. Kuroda"}]},{"@id":"https://cir.nii.ac.jp/crid/1380286991877815554","@type":"Researcher","foaf:name":[{"@value":"Y. Kasaba"}]},{"@id":"https://cir.nii.ac.jp/crid/1380286991877815553","@type":"Researcher","foaf:name":[{"@value":"N. Terada"}]},{"@id":"https://cir.nii.ac.jp/crid/1380286991877815552","@type":"Researcher","foaf:name":[{"@value":"H. Nakagawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1380286991877815555","@type":"Researcher","foaf:name":[{"@value":"K. Toriumi"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00191035"}],"prism:publicationName":[{"@value":"Icarus"}],"dc:publisher":[{"@value":"Elsevier BV"}],"prism:publicationDate":"2020-03","prism:volume":"338","prism:startingPage":"113567"},"reviewed":"false","dc:rights":["https://www.elsevier.com/tdm/userlicense/1.0/","https://www.elsevier.com/legal/tdmrep-license"],"url":[{"@id":"https://api.elsevier.com/content/article/PII:S0019103518300927?httpAccept=text/xml"},{"@id":"https://api.elsevier.com/content/article/PII:S0019103518300927?httpAccept=text/plain"}],"createdAt":"2019-11-27","modifiedAt":"2025-11-03","project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781911342080","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16K05552"},{"@type":"JGN","@value":"JP16K05552"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16K05552/"}],"notation":[{"@language":"ja","@value":"地表面から熱圏までをつないで気候変動に迫る，火星大気物理化学過程のモデリング研究"},{"@language":"en","@value":"Modeling study of the physical and chemical processes of Martian atmosphere connecting from the surface to thermosphere and approaching to the climate change"}]},{"@id":"https://cir.nii.ac.jp/crid/1040000781994904448","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"18H05439"},{"@type":"JGN","@value":"JP18H05439"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PLANNED-18H05439/"}],"notation":[{"@language":"ja","@value":"惑星大気の形成・進化とその多様性の解明"},{"@language":"en","@value":"Theoretical and Observational Studies of the Formation and Evolution of Diverse Planetary Atmospheres"}]},{"@id":"https://cir.nii.ac.jp/crid/1040000782017285120","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"19K03943"},{"@type":"JGN","@value":"JP19K03943"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-19K03943/"}],"notation":[{"@language":"ja","@value":"大気波動を介した下層大気から宇宙への物質輸送の研究"},{"@language":"en","@value":"Vertical transport from the lower atmosphere to space via atmospheric waves on Mars"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256872627712","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16H02229"},{"@type":"JGN","@value":"JP16H02229"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16H02229/"}],"notation":[{"@language":"ja","@value":"地球と火星の比較に基づく惑星電磁気圏環境に固有磁場強度が与える影響に関する研究"},{"@language":"en","@value":"Effects of intrinsic magnetic fields on the planetary magnetosphere/ionosphere environment based on comparison of Mars and Earth"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256990210944","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"19H00707"},{"@type":"JGN","@value":"JP19H00707"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-19H00707/"}],"notation":[{"@language":"ja","@value":"欧米探査機との協働で追う火星大気環境の変動と進化"},{"@language":"en","@value":"Variations and evolutions of Martian atmospheric environment investigated in the collaboration with European and US 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