{"@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/1363670319557919488.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/96ja02644"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F96JA02644"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/96JA02644"}}],"dc:title":[{"@value":"Theory of prominence eruption and propagation: Interplanetary consequences"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>The dynamics of solar magnetic flux ropes are investigated. The model starts with an equilibrium flux rope which contains a low‐density hot component and a denser cold component, qualitatively resembling a prominence cavity with an embedded prominence. The “eruption” of the entire flux rope is triggered by an increase in the poloidal magnetic flux of the structure. The subsequent expansion of the flux rope through a model corona and solar wind is analyzed using macroscopic quantities, including the forces, apex speed and height from the Sun, and magnetic field. The computed flux rope properties are in good agreement with those of observed magnetic clouds. On the basis of these results, magnetic clouds are identified as the interplanetary counterpart of the magnetic field and plasma of the initial cavity. The dense cold component, although drained out near the Sun, significantly influences the resulting magnetic structure in the heliosphere. After a cloud passes 1 AU, it is found that the magnetic field strength of the flux rope at 1 AU continues to decrease and that the magnetic energy in any finite heliocentric sphere vanishes as ∼<jats:italic>t</jats:italic><jats:sup>−1</jats:sup>, even with zero resistivity, where <jats:italic>t</jats:italic> is time. The cumulative magnetic energy inside the 1 AU sphere associated with repeated eruptions of flux ropes is calculated.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1383670319557919360","@type":"Researcher","foaf:name":[{"@value":"James Chen"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"1996-12","prism:volume":"101","prism:number":"A12","prism:startingPage":"27499","prism:endingPage":"27519"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F96JA02644"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/96JA02644"}],"createdAt":"2004-02-03","modifiedAt":"2023-09-22","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050845763733650304","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Kinematic Properties of Slow ICMEs and an Interpretation of a Modified Drag Equation for Fast and Moderate ICMEs"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002217423844608","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"EVOLUTION OF CORONAL MASS EJECTION MORPHOLOGY WITH INCREASING HELIOCENTRIC DISTANCE. 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GEOMETRICAL ANALYSIS"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002217424462976","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"MAGNETIC FIELD STRUCTURES TRIGGERING SOLAR FLARES AND CORONAL MASS EJECTIONS"}]},{"@id":"https://cir.nii.ac.jp/crid/1390282681490179456","@type":"Article","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"A self-similar solution of expanding cylindrical flux ropes for any polytropic index value"}]},{"@id":"https://cir.nii.ac.jp/crid/2050025942148522496","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Validation of coronal mass ejection arrival-time forecasts by magnetohydrodynamic simulations based on interplanetary scintillation observations"}]},{"@id":"https://cir.nii.ac.jp/crid/2050870367067472128","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Development of a coronal mass ejection arrival time forecasting system using interplanetary scintillation observations"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/96ja02644"},{"@type":"CROSSREF","@value":"10.1088/0004-637x/731/2/109_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"},{"@type":"CROSSREF","@value":"10.1088/0004-637x/760/1/31_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"},{"@type":"CROSSREF","@value":"10.1186/s40623-019-1019-5_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"},{"@type":"CROSSREF","@value":"10.1007/s11207-014-0472-3_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"},{"@type":"CROSSREF","@value":"10.1186/bf03351731_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"},{"@type":"CROSSREF","@value":"10.1186/s40623-020-01345-5_references_DOI_6QgjlYbulFK1sQ88P5mtVDhPaB7"}]}