{"@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/1361699994798264704.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2009je003380"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2009JE003380"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2009JE003380"}}],"dc:title":[{"@value":"Ages and stratigraphy of lunar mare basalts in Mare Frigoris and other nearside maria based on crater size‐frequency distribution measurements"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>We report on ages derived from impact crater counts for exposed mare basalt units in the northern part of the lunar nearside hemisphere (Mare Frigoris), the eastern and northeastern part of the nearside hemisphere (Lacus Temporis, Joliot, Hubble, Goddard, Mare Marginis, and Mare Smythii), the central part of the nearside hemisphere (Palus Putredinis, Mare Vaporum, and Sinus Medii), and the southwestern part of the nearside hemisphere (Grimaldi, Crüger, Rocca A, Lacus Aestatis, and Schickard). In Mare Frigoris, we dated 37 basalt units, showing ages from 2.61 to 3.77 Gyr, with most units being formed in the late Imbrian period between 3.4 and 3.8 Gyr ago. In Mare Vaporum we dated six spectrally homogeneous units that show model ages of 3.10 to 3.61 Gyr. Our model ages of basalts in Mare Marginis range from 3.38 to 3.88 Gyr and are mostly older than basalts in Mare Smythii (3.14–3.48 Gyr). The model ages of four units in Sinus Medii indicate that the basalts in this region formed 3.63 to 3.79 Gyr ago. We find an excellent agreement of our crater size‐frequency model ages of the Palus Putredinis area, which contains the Apollo 15 landing site, with the radiometric ages of Apollo 15 samples. According to our crater counts, basalts in Palus Putredinis are 3.34 Gyr old and this compares favorably with the radiometric ages of 3.30–3.35 Gyr of the olivine‐normative and quartz‐normative basalts of the Apollo 15 landing site. Lacus Aestatis is a small irregular‐shaped mare patch in the southwestern nearside and shows an Imbrian age of 3.50 Gyr; basalts in Lacus Temporis in the northeastern nearside formed between 3.62 and 3.74 Gyr ago and are, therefore, older than the basalts in Lacus Aestatis. We found that basalts in craters of the southwestern nearside (Schickard, Grimaldi, Crüger, and Rocca A) are also mostly younger than basalts in craters of the northeastern nearside (Hubble, Joliot, and Goddard). While basalt ages vary between 3.16 and 3.75 Gyr in the southwest, basalts in the northeast are 3.60–3.79 Gyr old. These results confirm and extend the general distribution of ages of mare basalt volcanism and further underline the predominance of older mare basalt ages in the eastern and southern nearside and in patches of mare peripheral to the larger maria, in contrast to the younger basalt ages on the western nearside (Oceanus Procellarum).</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380005521910511360","@type":"Researcher","foaf:name":[{"@value":"H. Hiesinger"}],"jpcoar:affiliationName":[{"@value":"Institut für Planetologie Westfälische Wilhelms‐Universität  Münster Germany"},{"@value":"Department of Geological Sciences Brown University  Providence Rhode Island USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994798264707","@type":"Researcher","foaf:name":[{"@value":"J. W. Head"}],"jpcoar:affiliationName":[{"@value":"Department of Geological Sciences Brown University  Providence Rhode Island USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994798264705","@type":"Researcher","foaf:name":[{"@value":"U. Wolf"}],"jpcoar:affiliationName":[{"@value":"DLR Institute of Planetary Exploration  Berlin Germany"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994798264706","@type":"Researcher","foaf:name":[{"@value":"R. Jaumann"}],"jpcoar:affiliationName":[{"@value":"DLR Institute of Planetary Exploration  Berlin Germany"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699994798264704","@type":"Researcher","foaf:name":[{"@value":"G. Neukum"}],"jpcoar:affiliationName":[{"@value":"Institut für Geologie, Geophysik und Geoinformatik Freie Universität Berlin  Berlin Germany"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Planets"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2010-03","prism:volume":"115","prism:number":"E3","prism:startingPage":"E03003"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2009JE003380"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2009JE003380"}],"createdAt":"2010-03-19","modifiedAt":"2023-11-02","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360002218091611520","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"An Automated Method for Crater Counting Using Rotational Pixel Swapping Method"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004229801309056","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Mare volcanism: Reinterpretation based on Kaguya Lunar Radar Sounder data"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283689326094592","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Surface vector mapping of magnetic anomalies over the Moon using Kaguya and Lunar Prospector observations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567182088618880","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Timing and characteristics of the latest mare eruption on the Moon"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567185751341056","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Magma source transition of lunar mare volcanism at 2.3 Ga"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848654737190784","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Lateral heterogeneity of lunar volcanic activity according to volumes of mare basalts in the farside basins"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848661184711424","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Lunar mare volcanism: lateral heterogeneities in volcanic activity and relationship with crustal structure"}]},{"@id":"https://cir.nii.ac.jp/crid/1360865814745892736","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The Structure and Evolution of the Lunar Interior"}]},{"@id":"https://cir.nii.ac.jp/crid/1361975843212930560","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Volcanic history in the Smythii basin based on SELENE radar observation"}]},{"@id":"https://cir.nii.ac.jp/crid/2051151842047696896","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Formation of ferroan dacite by lunar silicic volcanism recorded in a meteorite from the Moon"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2009je003380"},{"@type":"CROSSREF","@value":"10.1002/2013je004568_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1186/s40645-020-0324-8_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1109/tgrs.2017.2691758_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1002/2014je004785_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1111/maps.12896_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1002/2016je005246_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1144/sp401.11_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.2138/rmg.2023.89.06_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1038/s41598-019-50296-9_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"},{"@type":"CROSSREF","@value":"10.1016/j.epsl.2010.12.028_references_DOI_ItfF4Q3iv5sZEx6PNgewrVMYsB0"}]}