{"@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/1361699993735742080.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/2008ja013595"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2008JA013595"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2008JA013595"}}],"dc:title":[{"@value":"Physics‐based formula representations of high‐latitude ionospheric outflows: H<sup>+</sup> and O<sup>+</sup> densities, flow velocities, and temperatures versus soft electron precipitation, wave‐driven transverse heating, and solar zenith angle effects"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>Extensive systematic dynamic fluid kinetic (DyFK) model simulations are conducted to obtain advanced simulation‐based formula representations of ionospheric outflow parameters, for possible use by global magnetospheric modelers. Under F<jats:sub>10.7</jats:sub> levels of 142, corresponding to solar medium conditions, we obtain the H<jats:sup>+</jats:sup> and O<jats:sup>+</jats:sup> outflow densities, flow velocities, and perpendicular and parallel temperatures versus energy fluxes and characteristic energies of soft electron precipitation, wave spectral densities of ion transverse wave heating, and <jats:italic>F</jats:italic> region level solar zenith angle in the high‐latitude auroral region. From the results of hundreds of DyFK simulations of auroral outflows for ranges of each of these driving agents, we depict the H<jats:sup>+</jats:sup> and O<jats:sup>+</jats:sup> outflow density and flow velocity parameters at 3 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> altitude at the ends of these 2‐h simulation runs in spectrogram form versus various pairs of these influencing parameters. We further approximate these results by various distilled formula representations for the O<jats:sup>+</jats:sup> and H<jats:sup>+</jats:sup> outflow velocities, densities, and temperatures at 3 <jats:italic>R</jats:italic><jats:sub><jats:italic>E</jats:italic></jats:sub> altitude, as functions of the above indicated four “driver” parameters. These formula representations provide insight into the physics of these driven outflows, and may provide a convenient set of tools to set the boundary conditions for ionospheric plasma sources in global magnetospheric simulations.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380013168772453510","@type":"Researcher","foaf:name":[{"@value":"J. L. Horwitz"}],"jpcoar:affiliationName":[{"@value":"Department of Physics University of Texas at Arlington  Arlington Texas USA"}]},{"@id":"https://cir.nii.ac.jp/crid/1381699993735742080","@type":"Researcher","foaf:name":[{"@value":"W. Zeng"}],"jpcoar:affiliationName":[{"@value":"Department of Physics University of Texas at Arlington  Arlington Texas 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":"2009-01","prism:volume":"114","prism:number":"A1","prism:startingPage":"A01308"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2F2008JA013595"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2008JA013595"}],"createdAt":"2009-01-28","modifiedAt":"2023-10-31","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360285708263618432","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Observations of very‐low‐energy (<10 eV) ion outflows dominated by O<sup>+</sup> ions in the region of enhanced electron density in the polar cap magnetosphere during geomagnetic storms"}]},{"@id":"https://cir.nii.ac.jp/crid/1360298757416799104","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Nightside Auroral H<sup>+</sup> and O<sup>+</sup> Outflows Versus Energy Inputs During a Geomagnetic Storm"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567183243715456","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Storm‐time electron density enhancement in the cleft ion fountain"}]},{"@id":"https://cir.nii.ac.jp/crid/2051996266990212224","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"On the relationship between energy input to the ionosphere and the ion outflow flux under different solar zenith angles"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/2008ja013595"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01532-y_references_DOI_56zbErsZqNycsSKDf5dOCQFHKql"},{"@type":"CROSSREF","@value":"10.1029/2010ja015601_references_DOI_56zbErsZqNycsSKDf5dOCQFHKql"},{"@type":"CROSSREF","@value":"10.1029/2022ja030923_references_DOI_56zbErsZqNycsSKDf5dOCQFHKql"},{"@type":"CROSSREF","@value":"10.1029/2012ja017900_references_DOI_56zbErsZqNycsSKDf5dOCQFHKql"}]}