{"@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/1362825895639211776.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2002ja009739"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2002JA009739"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2002JA009739"}}],"dc:title":[{"@value":"Quiet time magnetotail plasma flow: Coordinated Polar ultraviolet images and Geotail observations"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>A search for fast flows in the plasma sheet during quiet times was conducted in order to further test the previously found close association between fast flows and auroral brightenings. We first identified “quiet intervals” of at least 30‐min duration in the Polar ultraviolet global images of auroras. During 16 months of Polar observations from January 1997 through April 1998, 41 quiet intervals were identified when Geotail was between 8 and 31 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> down the tail and within 10 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> of the midnight meridian. Fast flows were more rare during the quiet intervals than at other times. For 4 of the 41 intervals identified, Geotail detected flows faster than 300 km s<jats:sup>−1</jats:sup> in the plasma sheet. All the four flows were earthward parallel flows accompanied by northward magnetic field beyond 20 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub>, and there were no perpendicular flows faster than 300 km s<jats:sup>−1</jats:sup>. To understand the nature of the fast (but not perpendicular) flows during the quiet intervals, an earthward flow at 21 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> down the tail was studied in detail. The plasma beta was higher than unity during the earthward flow, but the fastest ion velocity moments consisted of the two counterstreaming components flowing along the magnetic field, a characteristic known to define the plasma sheet boundary layer. Our results further support the close association between auroral brightenings and clear fast flows as seen in previous studies, because no perpendicular fast flows were found during quiet intervals. Since some perpendicular flows slower than 300 km s<jats:sup>−1</jats:sup> were found beyond ∼20 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> down the tail, a velocity of ∼300 km s<jats:sup>−1</jats:sup> appears to statistically make a difference in the geoeffectiveness of perpendicular flows.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004236852866057","@type":"Researcher","foaf:name":[{"@value":"A. Ieda"}],"jpcoar:affiliationName":[{"@value":"Institute of Space and Astronautical Science  Sagamihara, Kanagawa Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492611","@type":"Researcher","foaf:name":[{"@value":"J.‐H. Shue"}],"jpcoar:affiliationName":[{"@value":"Applied Physics Laboratory Johns Hopkins University  Laurel Maryland USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492608","@type":"Researcher","foaf:name":[{"@value":"K. Liou"}],"jpcoar:affiliationName":[{"@value":"Applied Physics Laboratory Johns Hopkins University  Laurel Maryland USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492614","@type":"Researcher","foaf:name":[{"@value":"S.‐I. Ohtani"}],"jpcoar:affiliationName":[{"@value":"Applied Physics Laboratory Johns Hopkins University  Laurel Maryland USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492615","@type":"Researcher","foaf:name":[{"@value":"C.‐I. Meng"}],"jpcoar:affiliationName":[{"@value":"Applied Physics Laboratory Johns Hopkins University  Laurel Maryland USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492610","@type":"Researcher","foaf:name":[{"@value":"D. H. Fairfield"}],"jpcoar:affiliationName":[{"@value":"Laboratory for Extraterrestrial Physics NASA Goddard Space Flight Center  Greenbelt Maryland USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492616","@type":"Researcher","foaf:name":[{"@value":"T. Mukai"}],"jpcoar:affiliationName":[{"@value":"Institute of Space and Astronautical Science  Sagamihara, Kanagawa Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492617","@type":"Researcher","foaf:name":[{"@value":"Y. Saito"}],"jpcoar:affiliationName":[{"@value":"Institute of Space and Astronautical Science  Sagamihara, Kanagawa Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492609","@type":"Researcher","foaf:name":[{"@value":"S. Machida"}],"jpcoar:affiliationName":[{"@value":"Department of Geophysics Kyoto University  Kyoto Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492612","@type":"Researcher","foaf:name":[{"@value":"T. Nagai"}],"jpcoar:affiliationName":[{"@value":"Department of Earth and Planetary Sciences Tokyo Institute of Technology  Tokyo Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380579816115492613","@type":"Researcher","foaf:name":[{"@value":"G. K. Parks"}],"jpcoar:affiliationName":[{"@value":"Space Sciences Laboratory University of California  Berkeley California USA"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2003-09","prism:volume":"108","prism:number":"A9","prism:startingPage":"1345"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2002JA009739"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2002JA009739"}],"createdAt":"2003-09-12","modifiedAt":"2023-10-31","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360283691683877888","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Longitudinal association between magnetotail reconnection and auroral breakup based on Geotail and Polar observations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360869855566991744","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Duskward displacement of plasmoids and reconnection in the near-Earth magnetotail"}]},{"@id":"https://cir.nii.ac.jp/crid/2050588892078327552","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Visualization tool for three-dimensional plasma velocity distributions (ISEE_3D) as a plug-in for SPEDAS"}]},{"@id":"https://cir.nii.ac.jp/crid/2120589364340810112","@type":"OtherWorks","resourceType":"学術雑誌論文(journal article)","relationType":["isIdenticalTo"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Quiet Time Magnetotail Plasma Flow: Coordinated Polar Ultraviolet Images and GEOTAIL Observations"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2002ja009739"},{"@type":"OPENAIRE","@value":"doi_dedup___::67837ef68d2ecfab2e7ee2aa410f4b6e"},{"@type":"IRDB","@value":"oai:irdb.nii.ac.jp:01332:0004473693_isIdenticalTo_DOI_60IBMzl5AtGicSuUvmEjWjofzdL"},{"@type":"CROSSREF","@value":"10.1186/s40623-017-0761-9_references_DOI_Y0kq0USdGfZrDIm4s0SdsyeTebL"},{"@type":"CROSSREF","@value":"10.1029/2008ja013127_references_DOI_Y0kq0USdGfZrDIm4s0SdsyeTebL"},{"@type":"CROSSREF","@value":"10.1186/s40623-024-02003-w_references_DOI_Dv7SzT3rg95GCQLtY8KH9e48CF9"}]}