{"@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/1360574095749865472.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2005ja011251"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2005JA011251"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2005JA011251"}}],"dc:title":[{"@value":"Radial variations in the Io plasma torus during the Cassini era"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>A radial scan through the midnight sector of the Io plasma torus was made by the Cassini Ultraviolet Imaging Spectrograph on 14 January 2001, shortly after closest approach to Jupiter. From these data, Steffl et al. (2004a) derived electron temperature, plasma composition (ion mixing ratios), and electron column density as a function of radius from <jats:italic>L</jats:italic> = 6 to 9 as well as the total luminosity. We have advanced our homogeneous model of torus physical chemistry (Delamere and Bagenal, 2003) to include latitudinal and radial variations in a manner similar to the two‐dimensional model by Schreier et al. (1998). The model variables include: (1) neutral source rate, (2) radial transport coefficient, (3) the hot electron fraction, (4) hot electron temperature, and (5) the neutral O/S ratio. The radial variation of parameters 1–4 are described by simple power laws, making a total of nine parameters. We have explored the sensitivity of the model results to variations in these parameters and compared the best fit with previous Voyager era models (Schreier et al., 1998), Galileo data (Crary et al., 1998), and Cassini observations (Steffl et al., 2004a). We find that radial variations during the Cassini era are consistent with a neutral source rate of 700–1200 kg/s, an integrated transport time from <jats:italic>L</jats:italic> = 6 to 9 of 100–200 days, and that the core electron temperature is largely determined by a spatially and temporally varying superthermal electron population.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380306904383770246","@type":"Researcher","foaf:name":[{"@value":"P. A. Delamere"}],"jpcoar:affiliationName":[{"@value":"Laboratory for Atmospheric and Space Physics University of Colorado  Boulder Colorado USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380574095749865473","@type":"Researcher","foaf:name":[{"@value":"F. Bagenal"}],"jpcoar:affiliationName":[{"@value":"Laboratory for Atmospheric and Space Physics University of Colorado  Boulder Colorado USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1380574095749865474","@type":"Researcher","foaf:name":[{"@value":"A. Steffl"}],"jpcoar:affiliationName":[{"@value":"Department of Space Studies Southwest Research Institute  Boulder Colorado USA"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"2005-12","prism:volume":"110","prism:number":"A12"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2005JA011251"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2005JA011251"}],"createdAt":"2005-12-27","modifiedAt":"2023-10-31","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050001202716094592","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Response of Jupiter's Aurora to 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