{"@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/1361699995977292672.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/gl004i009p00377"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FGL004i009p00377"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/GL004i009p00377"}}],"dc:title":[{"@value":"Evidence for the control of Pc 3,4 magnetic pulsations by the solar wind velocity"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>The amplitude of Pc 3,4 magnetic pulsations at Calgary is shown to increase as the solar wind velocity increases. The pulsation amplitude dependence on solar wind velocity can be understood in terms of the Kelvin‐Helmholtz instability at the magnetopause boundary.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380025429408267548","@type":"Researcher","foaf:name":[{"@value":"H. J. Singer"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699995977292675","@type":"Researcher","foaf:name":[{"@value":"C. T. Russell"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699995977292674","@type":"Researcher","foaf:name":[{"@value":"M. G. Kivelson"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699995977292673","@type":"Researcher","foaf:name":[{"@value":"E. W. Greenstadt"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699995977292672","@type":"Researcher","foaf:name":[{"@value":"J. V. Olson"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00948276"},{"@type":"EISSN","@value":"19448007"}],"prism:publicationName":[{"@value":"Geophysical Research Letters"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"1977-09","prism:volume":"4","prism:number":"9","prism:startingPage":"377","prism:endingPage":"379"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FGL004i009p00377"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/GL004i009p00377"}],"createdAt":"2008-02-06","modifiedAt":"2023-09-23","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050576282633240832","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"A Statistical Study of the Solar Wind Dependence of Multi-Harmonic Toroidal ULF Waves Observed by the Arase Satellite"},{"@value":"A Statistical Study of the Solar Wind Dependence of Multi‐Harmonic Toroidal ULF Waves Observed by the Arase Satellite"}]},{"@id":"https://cir.nii.ac.jp/crid/1360025429408267904","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"From Foreshock 30-Second Waves to Magnetospheric Pc3 Waves"}]},{"@id":"https://cir.nii.ac.jp/crid/2050588891962944384","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Nighttime Pc3 pulsations : MM100 and MAGDAS observations"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/gl004i009p00377"},{"@type":"CROSSREF","@value":"10.1007/s11214-025-01152-y_references_DOI_VE9yiYlOXLsq7x8KXrouFRGXneD"},{"@type":"CROSSREF","@value":"10.1186/s40623-017-0647-x_references_DOI_VE9yiYlOXLsq7x8KXrouFRGXneD"},{"@type":"CROSSREF","@value":"10.1029/2021ja029840_references_DOI_VE9yiYlOXLsq7x8KXrouFRGXneD"}]}