{"@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/1050845763733650304.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"HDL","@value":"http://hdl.handle.net/2237/21224"}},{"identifier":{"@type":"URI","@value":"https://nagoya.repo.nii.ac.jp/records/19121"}},{"identifier":{"@type":"DOI","@value":"10.1007/s11207-014-0472-3"}},{"identifier":{"@type":"URI","@value":"http://link.springer.com/content/pdf/10.1007/s11207-014-0472-3.pdf"}},{"identifier":{"@type":"URI","@value":"http://link.springer.com/article/10.1007/s11207-014-0472-3/fulltext.html"}},{"identifier":{"@type":"URI","@value":"http://link.springer.com/content/pdf/10.1007/s11207-014-0472-3"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1401.1724"}},{"identifier":{"@type":"NAID","@value":"120005540274"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@language":"en","@value":"Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs"}],"dc:language":"en","description":[{"type":"Abstract","notation":[{"@language":"en","@value":"We report kinematic properties of slow interplanetary coronal mass ejections (ICMEs) identified by SOHO/LASCO, interplanetary scintillation, and in situ observations and propose a modified equation for the ICME motion. We identified seven ICMEs between 2010 and 2011 and compared them with 39 events reported in our previous work. We examined 15 fast (V SOHO−V bg>500 km s−1), 25 moderate (0 km s−1≤V SOHO−V bg≤500 km s−1), and 6 slow (V SOHO−V bg<0 km s−1) ICMEs, where V SOHO and V bg are the initial speed of ICMEs and the speed of the background solar wind. For slow ICMEs, we found the following results: i) They accelerate toward the speed of the background solar wind during their propagation and reach their final speed by 0.34±0.03 AU. ii) The acceleration ends when they reach 479±126 km s−1; this is close to the typical speed of the solar wind during the period of this study. iii) When γ 1 and γ 2 are assumed to be constants, a quadratic equation for the acceleration a=−γ 2(V−V bg)|V−V bg| is more appropriate than a linear one a=−γ 1(V−V bg), where V is the propagation speed of ICMEs, while the latter gives a smaller χ 2 value than the former. For the motion of the fast and moderate ICMEs, we found a modified drag equation a=−2.07×10−12(V−V bg)|V−V bg|−4.84×10−6(V−V bg). From the viewpoint of fluid dynamics, we interpret this equation as indicating that ICMEs with 0 km s−1≤V−V bg≤2300 km s−1 are controlled mainly by the hydrodynamic Stokes drag force, while the aerodynamic drag force is a predominant factor for the propagation of ICME with V−V bg>2300 km s−1."}]},{"type":"Other","notation":[{"@language":"en","@value":"Epub 2014 Jan 23."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1070845763733650304","@type":"Researcher","personIdentifier":[{"@type":"NRID","@value":"9000279888235"}],"foaf:name":[{"@language":"en","@value":"Iju, T."}]},{"@id":"https://cir.nii.ac.jp/crid/1070845763733650305","@type":"Researcher","personIdentifier":[{"@type":"NRID","@value":"9000279888236"}],"foaf:name":[{"@language":"en","@value":"Tokumaru, M."}]},{"@id":"https://cir.nii.ac.jp/crid/1070845763733650306","@type":"Researcher","personIdentifier":[{"@type":"NRID","@value":"9000279888237"}],"foaf:name":[{"@language":"en","@value":"Fujiki, K."}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00380938"},{"@type":"EISSN","@value":"1573093X"}],"prism:publicationName":[{"@language":"en","@value":"Solar Physics"}],"dc:publisher":[{"@value":"Springer"}],"prism:publicationDate":"2014-06","prism:volume":"289","prism:number":"6","prism:startingPage":"2157","prism:endingPage":"2175"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["The original publication is available at www.springerlink.com."],"url":[{"@id":"https://nagoya.repo.nii.ac.jp/records/19121"},{"@id":"http://link.springer.com/content/pdf/10.1007/s11207-014-0472-3.pdf"},{"@id":"http://link.springer.com/article/10.1007/s11207-014-0472-3/fulltext.html"},{"@id":"http://link.springer.com/content/pdf/10.1007/s11207-014-0472-3"},{"@id":"http://hdl.handle.net/2237/21224"}],"foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Coronal%20mass%20ejections","dc:title":"Coronal mass ejections"},{"@id":"https://cir.nii.ac.jp/all?q=Interplanetary%20coronal%20mass%20ejections","dc:title":"Interplanetary coronal mass ejections"},{"@id":"https://cir.nii.ac.jp/all?q=Plasma%20physics","dc:title":"Plasma physics"},{"@id":"https://cir.nii.ac.jp/all?q=Radio%20scintillation","dc:title":"Radio scintillation"}],"dcterms:subject":[{"subjectScheme":"Other","notation":[{"@value":"Coronal mass ejections"}]},{"subjectScheme":"Other","notation":[{"@value":"Interplanetary coronal mass ejections"}]},{"subjectScheme":"Other","notation":[{"@value":"Plasma physics"}]},{"subjectScheme":"Other","notation":[{"@value":"Radio scintillation"}]}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040000782238634112","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"25247079"},{"@type":"JGN","@value":"JP25247079"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-25247079/"}],"notation":[{"@language":"ja","@value":"特異な太陽ダイナモ活動に伴う太陽圏全体構造の変動の解明"},{"@language":"en","@value":"Study of structural variation of the global heliosphere associated with the peculiar solar dynamo activity"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050282813779251584","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Radial Speed Evolution of Interplanetary Coronal Mass Ejections During Solar Cycle 23"},{"@value":"Radial speed evolution of coronal mass ejections during solar cycle 23"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004233289579648","@type":"Article","resourceType":"学術雑誌論文(journal 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