{"@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/1362825893406281728.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2001ja000023"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2001JA000023"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2001JA000023"}}],"dc:title":[{"@value":"Multistep <i>Dst</i> development and ring current composition changes during the 4–6 June 1991 magnetic storm"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>The 4–6 June 1991 magnetic storm, which occurred during solar maximum conditions, is analyzed to investigate two observed features of magnetic storms that are not completely understood: (1) the mass‐dependent decay of the ring current during the early recovery phase and (2) the role of preconditioning in multistep ring current development. A kinetic ring current drift‐loss model, driven by dynamic fluxes at the nightside outer boundary, was used to simulate this storm interval. A strong partial ring current developed and persisted throughout the main and early recovery phases. The majority of ions in the partial ring current make one pass through the inner magnetosphere on open drift paths before encountering the dayside magnetopause. The ring current exhibited a three‐phase decay in this storm. A short interval of charge‐exchange loss constituted the first phase of the decay followed by a classical two‐phase decay characterized by an abrupt transition between two very different decay timescales. The short interval dominated by charge‐exchange loss occurred because an abrupt northward turning of the interplanetary magnetic field (IMF) trapped ring current ions on closed trajectories, and turned‐off sources and “flow‐out” losses. If this had been the end of the solar wind disturbance, decay timescales would have gradually lengthened as charge exchange preferentially removed the short‐lived species; a distinctive two‐phase decay would not have resulted. However, the IMF turned weakly southward, drift paths became open, and a standard two‐phase decay ensued as the IMF rotated slowly northward again. As has been shown before, a two‐phase decay is produced as open drift paths are converted to closed in a weakening convection electric field, driving a transition from the fast flow‐out losses associated with the partial ring current to the slower charge‐exchange losses associated with the trapped ring current. The open drift path geometry during the main phase and during phase 1 of the two‐phase decay has important consequences for the evolution of ring current composition and for preconditioning issues. In this particular storm, ring current composition changes measured by the Combined Release and Radiation Effects Satellite (CRRES) during the main and recovery phase of the storm resulted largely from composition changes in the plasma sheet transmitted into the inner magnetosphere along open drift paths as the magnetic activity declined. Possible preconditioning elements were investigated during the multistep development of this storm, which was driven by the sequential arrival of three southward IMF <jats:italic>B</jats:italic><jats:sub><jats:italic>z</jats:italic></jats:sub> intervals of increasing peak strength. In each case, previous intensifications (preexisting ring currents) were swept out of the magnetosphere by the enhanced convection associated with the latest intensification and did not act as a significant preconditioning element. However, plasma sheet characteristics varied significantly between subsequent intensifications, altering the response of the magnetosphere to the sequential solar wind drivers. A denser plasma sheet (ring current source population) appeared during the second intensification, compensating for the weaker IMF <jats:italic>B</jats:italic><jats:sub><jats:italic>z</jats:italic></jats:sub> at this time and producing a minimum pressure‐corrected <jats:italic>Dst</jats:italic>* value comparable to the third intensification (driven by stronger IMF <jats:italic>B</jats:italic><jats:sub><jats:italic>z</jats:italic></jats:sub> but a lower density plasma sheet source). The controlling influence of the plasma sheet dynamics on the ring current dynamics and its role in altering the inner magnetospheric response to solar wind drivers during magnetic storms adds a sense of urgency to understanding what processes produce time‐dependent responses in the plasma sheet density, composition, and temperature.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380567186806646272","@type":"Researcher","foaf:name":[{"@value":"J. U. Kozyra"}],"jpcoar:affiliationName":[{"@value":"Space Physics Research Laboratory University of Michigan  Ann Arbor Michigan USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281732","@type":"Researcher","foaf:name":[{"@value":"M. W. Liemohn"}],"jpcoar:affiliationName":[{"@value":"Space Physics Research Laboratory University of Michigan  Ann Arbor Michigan USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281733","@type":"Researcher","foaf:name":[{"@value":"C. R. Clauer"}],"jpcoar:affiliationName":[{"@value":"Space Physics Research Laboratory University of Michigan  Ann Arbor Michigan USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281730","@type":"Researcher","foaf:name":[{"@value":"A. J. Ridley"}],"jpcoar:affiliationName":[{"@value":"Space Physics Research Laboratory University of Michigan  Ann Arbor Michigan USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281731","@type":"Researcher","foaf:name":[{"@value":"M. F. Thomsen"}],"jpcoar:affiliationName":[{"@value":"Space and Atmospheric Science Division Los Alamos National Laboratory  Los Alamos New Mexico USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281728","@type":"Researcher","foaf:name":[{"@value":"J. E. Borovsky"}],"jpcoar:affiliationName":[{"@value":"Space and Atmospheric Science Division Los Alamos National Laboratory  Los Alamos New Mexico USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281736","@type":"Researcher","foaf:name":[{"@value":"J. L. Roeder"}],"jpcoar:affiliationName":[{"@value":"The Aerospace Corporation  El Segundo California USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281729","@type":"Researcher","foaf:name":[{"@value":"V. K. Jordanova"}],"jpcoar:affiliationName":[{"@value":"Space Science Center University of New Hampshire  Durham New Hampshire USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825893406281734","@type":"Researcher","foaf:name":[{"@value":"W. D. Gonzalez"}],"jpcoar:affiliationName":[{"@value":"Instituto de Pesquisas Especiais São José dos Campos  São Paulo Brazil"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2002-08","prism:volume":"107","prism:number":"A8","prism:startingPage":"1"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2001JA000023"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2001JA000023"}],"createdAt":"2002-10-27","modifiedAt":"2023-10-31","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050282677278592512","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Magnetic field depression at the Earth's surface during energetic neutral atom emission fade-out in the inner magnetosphere"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002214351443328","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Three‐Step Buildup of the 17 March 2015 Storm Ring Current: Implication for the Cause of the Unexpected Storm Intensification"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004233286919680","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Evolution of ring current ion energy spectra during the storm recovery phase: Implication for dominant ion loss processes"}]},{"@id":"https://cir.nii.ac.jp/crid/1360021390558309120","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Plasma Pressure Distribution of Ions and Electrons in the Inner Magnetosphere During CIR Driven Storms Observed During Arase Era"}]},{"@id":"https://cir.nii.ac.jp/crid/1360021391857264000","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The RAM-SCB model and its applications to advance space weather forecasting"}]},{"@id":"https://cir.nii.ac.jp/crid/1360584341827566976","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Relativistic electron flux growth during storm and non-storm periods as observed by ARASE and GOES satellites"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848656365423616","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"A Review of General Physical and Chemical Processes Related to Plasma Sources and Losses for Solar System Magnetospheres"}]},{"@id":"https://cir.nii.ac.jp/crid/2050588892089878144","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Characteristics of storm time ion composition in the near-Earth plasma sheet using Geotail and RBSP measurements"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2001ja000023"},{"@type":"CROSSREF","@value":"10.1002/2017ja024462_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1029/2010ja015628_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1029/2023ja031756_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1016/j.asr.2022.08.077_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1029/2010ja015799_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1186/s40623-018-0977-3_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1186/s40623-023-01925-1_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"},{"@type":"CROSSREF","@value":"10.1007/s11214-015-0170-y_references_DOI_WsalblvYy8IajbUsTXLFgTxKf2k"}]}