{"@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/1364233268790625280.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/te038i002p00079"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FTE038i002p00079"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/TE038i002p00079"}}],"dc:title":[{"@value":"A new theory of magnetic storms"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>10.1—The distortion of the front surface of the stream produced by the magnetic field as the stream advances towards the Earth has been described briefly in §§6.6 and 7.7; as was there mentioned, we have not discussed in detail the shape of the hollow formed, or the subsequent phenomena occurring therein. We defer this consideration until we have a clearer understanding of the mode in which the ions near the surface of the stream are able to advance into the Earth's field. But certain general features can be deduced, as has been pointed out already in §1.8; the hollow gradually shrinks at a diminishing rate, but we cannot say at present whether it ultimately closes in upon the earth. The preceding analysis suggests that once the velocity of the particles is diminished to, say, 1/10 of its initial value (10<jats:sup>8</jats:sup> cm/sec), the rate at which the hollow closes up becomes slow.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004236852388612","@type":"Researcher","foaf:name":[{"@value":"S. Chapman"}]},{"@id":"https://cir.nii.ac.jp/crid/1384233268790625281","@type":"Researcher","foaf:name":[{"@value":"V. C. A. Ferraro"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00968013"},{"@type":"EISSN","@value":"00968013"}],"prism:publicationName":[{"@value":"Terrestrial Magnetism and Atmospheric Electricity"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"1933-06","prism:volume":"38","prism:number":"2","prism:startingPage":"79","prism:endingPage":"96"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FTE038i002p00079"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/TE038i002p00079"}],"createdAt":"2008-02-06","modifiedAt":"2023-09-22","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050845760765770752","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Relationship between solar wind dynamic pressure and amplitude of geomagnetic sudden commencement (SC)"}]},{"@id":"https://cir.nii.ac.jp/crid/1360306906103144704","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Science highlights from the Kjell Henriksen Observatory on Svalbard"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848655764317824","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Dynamic Inner Magnetosphere: A Tutorial and Recent Advances"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/te038i002p00079"},{"@type":"CROSSREF","@value":"10.1186/s40623-016-0444-y_references_DOI_3jA0HsnnW0yMonPhNwuNYwtXMWJ"},{"@type":"CROSSREF","@value":"10.1139/as-2024-0009_references_DOI_3jA0HsnnW0yMonPhNwuNYwtXMWJ"},{"@type":"CROSSREF","@value":"10.1007/978-94-007-0501-2_9_references_DOI_3jA0HsnnW0yMonPhNwuNYwtXMWJ"}]}