Magnetic Flux Circulation in the Saturnian Magnetosphere as Constrained by Cassini Observations in the Inner Magnetosphere.
Saved in:
| Title: | Magnetic Flux Circulation in the Saturnian Magnetosphere as Constrained by Cassini Observations in the Inner Magnetosphere. |
|---|---|
| Authors: | Lai, Hairong1 laihr@mail.sysu.edu.cn, Jia, Ying‐Dong2, Russell, Christopher T.2, Jia, Xianzhe3, Masters, Adam4, Dougherty, Michele K.4, Cui, Jun1 |
| Source: | Journal of Geophysical Research. Space Physics. Nov2021, Vol. 126 Issue 11, p1-9. 9p. |
| Subject Terms: | Magnetic flux, Magnetosphere, Atmosphere of Saturn, Curvature |
| Company/Entity: | Cassini (Spacecraft) |
| Abstract: | In steady state, magnetic flux conservation must be maintained in Saturn's magnetosphere. The Enceladus plumes add mass to magnetic flux tubes in the inner magnetosphere, and centrifugal force pulls the mass‐loaded flux tubes outward. Those flux tubes are carried outward to the magnetotail where they deposit their mass and return to the mass loading region. It may take days for the magnetic flux to be carried outward to the tail, but the return of the nearly empty flux tubes can last only several hours, with speeds of inward motion around 200 km/s. Using time sequences of Cassini particle count rate, the difference in curvature drift and gradient drift is accounted for to determine the return speed, age, and starting dipole L‐shell of return flux tubes. Determination of this flux‐return process improves our understanding of the magnetic flux circulation at Saturn and provides insight into how other giant planets remove the mass added by their moons. Key Points: To determine the flux return process, the count rate distributions of ions/electrons inside a flux tube have been studiedWe use a stretched dipolar magnetosphere model and account for the difference in curvature and gradient driftWe estimate the starting dipole L shell of the return flux tubes to be greater than 45 [ABSTRACT FROM AUTHOR] |
| Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.) | |
| Database: | GreenFILE |
| FullText | Text: Availability: 0 |
|---|---|
| Header | DbId: 8gh DbLabel: GreenFILE An: 153749448 AccessLevel: 6 PubType: Academic Journal PubTypeId: academicJournal PreciseRelevancyScore: 0 |
| IllustrationInfo | |
| Items | – Name: Title Label: Title Group: Ti Data: Magnetic Flux Circulation in the Saturnian Magnetosphere as Constrained by Cassini Observations in the Inner Magnetosphere. – Name: Author Label: Authors Group: Au Data: <searchLink fieldCode="AR" term="%22Lai%2C+Hairong%22">Lai, Hairong</searchLink><relatesTo>1</relatesTo><i> laihr@mail.sysu.edu.cn</i><br /><searchLink fieldCode="AR" term="%22Jia%2C+Ying‐Dong%22">Jia, Ying‐Dong</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Russell%2C+Christopher+T%2E%22">Russell, Christopher T.</searchLink><relatesTo>2</relatesTo><br /><searchLink fieldCode="AR" term="%22Jia%2C+Xianzhe%22">Jia, Xianzhe</searchLink><relatesTo>3</relatesTo><br /><searchLink fieldCode="AR" term="%22Masters%2C+Adam%22">Masters, Adam</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22Dougherty%2C+Michele+K%2E%22">Dougherty, Michele K.</searchLink><relatesTo>4</relatesTo><br /><searchLink fieldCode="AR" term="%22Cui%2C+Jun%22">Cui, Jun</searchLink><relatesTo>1</relatesTo> – Name: TitleSource Label: Source Group: Src Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Space+Physics%22">Journal of Geophysical Research. Space Physics</searchLink>. Nov2021, Vol. 126 Issue 11, p1-9. 9p. – Name: Subject Label: Subject Terms Group: Su Data: <searchLink fieldCode="DE" term="%22Magnetic+flux%22">Magnetic flux</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetosphere%22">Magnetosphere</searchLink><br /><searchLink fieldCode="DE" term="%22Atmosphere+of+Saturn%22">Atmosphere of Saturn</searchLink><br /><searchLink fieldCode="DE" term="%22Curvature%22">Curvature</searchLink> – Name: SubjectCompany Label: Company/Entity Group: Su Data: <searchLink fieldCode="DE" term="%22Cassini+%28Spacecraft%29%22">Cassini (Spacecraft)</searchLink> – Name: Abstract Label: Abstract Group: Ab Data: In steady state, magnetic flux conservation must be maintained in Saturn's magnetosphere. The Enceladus plumes add mass to magnetic flux tubes in the inner magnetosphere, and centrifugal force pulls the mass‐loaded flux tubes outward. Those flux tubes are carried outward to the magnetotail where they deposit their mass and return to the mass loading region. It may take days for the magnetic flux to be carried outward to the tail, but the return of the nearly empty flux tubes can last only several hours, with speeds of inward motion around 200 km/s. Using time sequences of Cassini particle count rate, the difference in curvature drift and gradient drift is accounted for to determine the return speed, age, and starting dipole L‐shell of return flux tubes. Determination of this flux‐return process improves our understanding of the magnetic flux circulation at Saturn and provides insight into how other giant planets remove the mass added by their moons. Key Points: To determine the flux return process, the count rate distributions of ions/electrons inside a flux tube have been studiedWe use a stretched dipolar magnetosphere model and account for the difference in curvature and gradient driftWe estimate the starting dipole L shell of the return flux tubes to be greater than 45 [ABSTRACT FROM AUTHOR] – Name: AbstractSuppliedCopyright Label: Group: Ab Data: <i>Copyright of Journal of Geophysical Research. Space Physics is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.) |
| PLink | https://search.ebscohost.com/login.aspx?direct=true&site=eds-live&db=8gh&AN=153749448 |
| RecordInfo | BibRecord: BibEntity: Identifiers: – Type: doi Value: 10.1029/2021JA029304 Languages: – Code: eng Text: English PhysicalDescription: Pagination: PageCount: 9 StartPage: 1 Subjects: – SubjectFull: Magnetic flux Type: general – SubjectFull: Magnetosphere Type: general – SubjectFull: Atmosphere of Saturn Type: general – SubjectFull: Curvature Type: general – SubjectFull: Cassini (Spacecraft) Type: general Titles: – TitleFull: Magnetic Flux Circulation in the Saturnian Magnetosphere as Constrained by Cassini Observations in the Inner Magnetosphere. Type: main BibRelationships: HasContributorRelationships: – PersonEntity: Name: NameFull: Lai, Hairong – PersonEntity: Name: NameFull: Jia, Ying‐Dong – PersonEntity: Name: NameFull: Russell, Christopher T. – PersonEntity: Name: NameFull: Jia, Xianzhe – PersonEntity: Name: NameFull: Masters, Adam – PersonEntity: Name: NameFull: Dougherty, Michele K. – PersonEntity: Name: NameFull: Cui, Jun IsPartOfRelationships: – BibEntity: Dates: – D: 01 M: 11 Text: Nov2021 Type: published Y: 2021 Identifiers: – Type: issn-print Value: 21699380 Numbering: – Type: volume Value: 126 – Type: issue Value: 11 Titles: – TitleFull: Journal of Geophysical Research. Space Physics Type: main |
| ResultId | 1 |
