{"@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/1363388846350428544.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1002/2016je005175"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1002%2F2016JE005175"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2016JE005175"}}],"dc:title":[{"@value":"Escape and evolution of Mars's CO<sub>2</sub> atmosphere: Influence of suprathermal atoms"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title><jats:p>With a Monte Carlo model we investigate the escape of hot oxygen and carbon from the Martian atmosphere for four points in time in its history corresponding to 1, 3, 10, and 20 times the present solar EUV flux. We study and discuss different sources of hot oxygen and carbon atoms in the thermosphere and their changing importance with the EUV flux. The increase of the production rates due to higher densities resulting from the higher EUV flux competes against the expansion of the thermosphere and corresponding increase in collisions. We find that the escape due to photodissociation increases with increasing EUV level. However, for the escape via some other reactions, e.g., dissociative recombination of \n<jats:inline-graphic xmlns:xlink=\"http://www.w3.org/1999/xlink\" xlink:href=\"graphic/jgre20682-math-0001.png\" xlink:title=\"urn:x-wiley:jgre:media:jgre20682:jgre20682-math-0001\"/>, this is only true until the EUV level reaches 10 times the present EUV flux and then the rates start to decrease. Furthermore, our results show that Mars could not have had a dense atmosphere at the end of the Noachian epoch, since such an atmosphere would not have been able to escape until today. In the pre‐Noachian era, most of the magma ocean and volcanic activity‐related outgassed CO<jats:sub>2</jats:sub> atmosphere could have been lost thermally until the Noachian epoch, when nonthermal loss processes such as suprathermal atom escape became dominant. Thus, early Mars could have been hot and wet during the pre‐Noachian era with surface CO<jats:sub>2</jats:sub> pressures larger than 1 bar during the first 300 Myr after the planet's origin.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380021391873340692","@type":"Researcher","foaf:name":[{"@value":"U. V. Amerstorfer"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute Austrian Academy of Sciences  Graz Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428673","@type":"Researcher","foaf:name":[{"@value":"H. Gröller"}],"jpcoar:affiliationName":[{"@value":"Lunar and Planetary Laboratory University of Arizona  Tucson Arizona USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428672","@type":"Researcher","foaf:name":[{"@value":"H. Lichtenegger"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute Austrian Academy of Sciences  Graz Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428677","@type":"Researcher","foaf:name":[{"@value":"H. Lammer"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute Austrian Academy of Sciences  Graz Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428544","@type":"Researcher","foaf:name":[{"@value":"F. Tian"}],"jpcoar:affiliationName":[{"@value":"Ministry of Education Key Laboratory for Earth System Modeling, Center for Earth System Science Tsinghua University  Beijing China"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428674","@type":"Researcher","foaf:name":[{"@value":"L. Noack"}],"jpcoar:affiliationName":[{"@value":"Royal Observatory of Belgium  Brussels Belgium"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428675","@type":"Researcher","foaf:name":[{"@value":"M. Scherf"}],"jpcoar:affiliationName":[{"@value":"Space Research Institute Austrian Academy of Sciences  Graz Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428545","@type":"Researcher","foaf:name":[{"@value":"C. Johnstone"}],"jpcoar:affiliationName":[{"@value":"Department of Astrophysics University of Vienna  Vienna Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428678","@type":"Researcher","foaf:name":[{"@value":"L. Tu"}],"jpcoar:affiliationName":[{"@value":"Department of Astrophysics University of Vienna  Vienna Austria"}]},{"@id":"https://cir.nii.ac.jp/crid/1383388846350428676","@type":"Researcher","foaf:name":[{"@value":"M. Güdel"}],"jpcoar:affiliationName":[{"@value":"Department of Astrophysics University of Vienna  Vienna Austria"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"21699097"},{"@type":"EISSN","@value":"21699100"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Planets"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2017-06","prism:volume":"122","prism:number":"6","prism:startingPage":"1321","prism:endingPage":"1337"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1002%2F2016JE005175"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1002/2016JE005175"}],"createdAt":"2017-05-24","modifiedAt":"2023-10-04","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/1360021391873340800","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Atmospheric formaldehyde production on early Mars leading to a potential formation of bio-important molecules"}]},{"@id":"https://cir.nii.ac.jp/crid/1360572092871511936","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Loss and Fractionation of Noble Gas Isotopes and Moderately Volatile Elements from Planetary Embryos and Early Venus, Earth and Mars"}]},{"@id":"https://cir.nii.ac.jp/crid/1360588380587933568","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Stable carbon isotope evolution of formaldehyde on early Mars"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848657114616832","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1002/2016je005175"},{"@type":"CROSSREF","@value":"10.1038/s41598-024-52718-9_references_DOI_O9MiFk0PkmP3WgGbVzJVwlbpIwk"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2018.05.030_references_DOI_O9MiFk0PkmP3WgGbVzJVwlbpIwk"},{"@type":"CROSSREF","@value":"10.1007/s11214-020-00701-x_references_DOI_O9MiFk0PkmP3WgGbVzJVwlbpIwk"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01417-0_references_DOI_O9MiFk0PkmP3WgGbVzJVwlbpIwk"},{"@type":"CROSSREF","@value":"10.1038/s41598-024-71301-w_references_DOI_O9MiFk0PkmP3WgGbVzJVwlbpIwk"}]}