{"@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/1362825896120472192.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1029/ja086ia13p11401"}},{"identifier":{"@type":"URI","@value":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FJA086iA13p11401"}},{"identifier":{"@type":"URI","@value":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA086iA13p11401"}},{"identifier":{"@type":"NAID","@value":"30034750476"}}],"dc:title":[{"@value":"Solar wind flow about the terrestrial planets 1. Modeling bow shock position and shape"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:p>General technique for modeling the position and shape of planetary bow waves are reviewed. A three‐parameter method was selected to model the near portion (i.e.,<jats:italic>x</jats:italic>′ > −1 <jats:italic>R<jats:sub>ob</jats:sub></jats:italic>) of the Venus, earth, and Mars bow shocks and the results compared with existing models using 1 to 6 free variables. By limiting consideration to the forward part of the bow wave, only the region of the shock surface that is most sensitive to obstacle shape and size was examined. In contrast, most other studies include portions of the more distant downstream shock, thus tending to reduce the planetary magnetosphere in question to a point source and constrain the resultant model surfaces to be paraboloid or hyperboloid in shape to avoid downstream closure. It was found by this investigation that the relative effective shapes of the near Martian, Cytherean, and terrestrial bow shocks are ellipsoidal, paraboloidal, and hyperboloidal, respectively, in response to the increasing bluntness of the obstacles that Mars, Venus, and earth present to the solar wind. The position of the terrestrial shock over the years 1965 to 1972 showed only a weak dependence on the phase of the solar cycle after the effects of solar wind dynamic pressure on magnetopause location were taken into account. However, the bow wave of Venus was considerably more distant around solar maximum in 1979 than at minimum in 1975–6 suggesting a solar cycle variation in its interaction with the solar wind. Finally, no significant deviations from axial symmetry were found when the near bow waves of the earth and Venus were mapped into the aberrated terminator plane. This finding is in agreement with the predictions of gas dynamic theory which neglects the effects of the IMF on the grounds of their smallness. Farther downstream where the bow wave position is being limited by the MHD fast mode Mach cone, an elliptical cross section is expected and noted in the results of other investigations.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1382825896120472193","@type":"Researcher","foaf:name":[{"@value":"James A. Slavin"}]},{"@id":"https://cir.nii.ac.jp/crid/1382825896120472192","@type":"Researcher","foaf:name":[{"@value":"Robert E. Holzer"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"01480227"}],"prism:publicationName":[{"@value":"Journal of Geophysical Research: Space Physics"}],"dc:publisher":[{"@value":"American Geophysical Union (AGU)"}],"prism:publicationDate":"1981-12","prism:volume":"86","prism:number":"A13","prism:startingPage":"11401","prism:endingPage":"11418"},"reviewed":"false","dc:rights":["http://onlinelibrary.wiley.com/termsAndConditions#vor"],"url":[{"@id":"https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1029%2FJA086iA13p11401"},{"@id":"https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/JA086iA13p11401"}],"createdAt":"2008-02-06","modifiedAt":"2023-09-22","relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360025430178137088","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Complex Interaction of Reconnected Field Lines at Earth's Magnetopause Under Sub‐Alfvénic Solar Wind With Northward Magnetic Field"}]},{"@id":"https://cir.nii.ac.jp/crid/1360294643708714496","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"BepiColombo Science Investigations During Cruise and Flybys at the Earth, Venus and Mercury"}]},{"@id":"https://cir.nii.ac.jp/crid/1360298757422127360","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Asymmetric deformation of the Earth’s magnetosphere under low Alfvén Mach number solar wind: Observations and MHD simulation"}]},{"@id":"https://cir.nii.ac.jp/crid/1360302865556130944","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Direct evidence of substorm-related impulsive injections of electrons at Mercury"}]},{"@id":"https://cir.nii.ac.jp/crid/1360567181545127296","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Electric Solar Wind Sail Kinetic Energy Impactor for Asteroid Deflection Missions"}]},{"@id":"https://cir.nii.ac.jp/crid/1360576118699648256","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Comparative Na and K Mercury and Moon Exospheres"}]},{"@id":"https://cir.nii.ac.jp/crid/1360846640879672192","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Electrons on closed field lines of lunar crustal fields in the solar wind wake"}]},{"@id":"https://cir.nii.ac.jp/crid/1360848657114572672","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Kaguya observations of the lunar wake in the terrestrial foreshock: Surface potential change by bow-shock reflected ions"}]},{"@id":"https://cir.nii.ac.jp/crid/1361975841429748352","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Orbital maneuvering of electric solar wind sail based on an advanced solar wind force model"}]},{"@id":"https://cir.nii.ac.jp/crid/1390001206509779072","@type":"Article","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Three-dimensional hybrid simulation of magnetized plasma flow around an obstacle"}]},{"@id":"https://cir.nii.ac.jp/crid/1390001206510962688","@type":"Article","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"The PLANET-B mission"}]},{"@id":"https://cir.nii.ac.jp/crid/1390001206513258112","@type":"Article","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Wind observations of the terrestrial bow shock"},{"@value":"Wind observations of the terrestrial bow shock: 3-D shape and motion"}]},{"@id":"https://cir.nii.ac.jp/crid/1523388080704510464","@type":"Article","relationType":["isCitedBy"],"jpcoar:relatedTitle":[{"@value":"Wind observations of the terrestrial bow shock: 3-D shape and motion"},{"@language":"ja-Kana","@value":"Wind observations of the terrestrial bow shock 3 D shape and motion"}]},{"@id":"https://cir.nii.ac.jp/crid/2051996266990221824","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"An event study on broadband electric field noises and electron distributions in the lunar wake boundary"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1029/ja086ia13p11401"},{"@type":"CIA","@value":"30034750476"},{"@type":"CROSSREF","@value":"10.1186/bf03352242_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1029/2024ja033395_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2014.12.007_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1007/s11214-021-00797-9_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1186/s40623-022-01744-w_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1038/s41467-023-39565-4_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1186/bf03351697_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1186/bf03352100_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1007/s40295-015-0081-x_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1016/j.icarus.2017.04.005_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1016/j.actaastro.2019.10.001_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1007/s11214-022-00871-w_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"},{"@type":"CROSSREF","@value":"10.1186/s40623-021-01566-2_references_DOI_GuWxh9v5voIyEqMzdDFqGwJfO0Q"}]}