Different Faces of the Martian Magnetosphere.
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| Title: | Different Faces of the Martian Magnetosphere. |
|---|---|
| Authors: | Dubinin, E.1 (AUTHOR) dubinin@mps.mpg.de, Fraenz, M.1 (AUTHOR), Modolo, R.2 (AUTHOR), Pätzold, M.3 (AUTHOR), Tellmann, S.3 (AUTHOR), DiBraccio, G.4 (AUTHOR) |
| Source: | Journal of Geophysical Research. Space Physics. Apr2025, Vol. 130 Issue 4, p1-16. 16p. |
| Subject Terms: | Interplanetary magnetic fields, Solar magnetic fields, Magnetic dipoles, Magnetosphere, Orbits (Astronomy), Solar wind |
| Abstract: | The Martian magnetosphere contains components of the induced and intrinsic magnetospheres. Since we can not get a global snapshot of the magnetosphere we use a statistical picture based on a large number of measurements. Depending on the choice of coordinate system and the data selection we can observe different faces of the Martian magnetosphere. If we map data in the Martian Solar Electric coordinate system, then we can separate the induced features of the magnetosphere which appears similar to the magnetosphere of Venus. If we use the Martian Solar Orbital coordinate system and select together the orbits with positive and negative By ${B}_{y}$‐component of the IMF, then the effects related to draped magnetic field and the high order harmonics of the crustal magnetic field are significantly weakened because of averaging over many orbits and a dipole‐like magnetosphere of Mars becomes visible. If we select separately the orbits with positive and negative By ${B}_{y}$‐component we observe a twist of the magnetotail in the direction determined by the sign of By ${B}_{y}$ that is typical for a hybrid magnetosphere with the induced and intrinsic components. The intrinsic and induced components are also well separated when we select the orbits with northward IMF. Then we observe the features that are somewhat similar to those at the Earth magnetosphere. When we use the MSO coordinates and separate by the phase of Mars rotation, the tail topology occurs more complex. This indicates that the effects of the local crustal magnetic field turn out as being also important. Plain Language Summary: The Martian magnetosphere contains features typical for induced and intrinsic magnetospheres. To describe these features we use a picture based on a statistical approach with a large number of measurements. It was shown that utilizing different coordinate systems and selecting orbits with different cross‐flow components of the interplanetary magnetic field in the solar wind we can separate the induced and intrinsic components inherent to the Martian magnetosphere. We can isolate the induced component and observe the features that are in many ways similar to those we see at Venus. Isolating the intrinsic component we have found a dipole‐like obstacle for solar wind. Key Points: The Martian ionosphere contains components of the induced and intrinsic magnetospheresUsing different coordinate systems and averaging on the different data set we can separate these componentsA dipole‐like obstacle for solar wind is revealed [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.) | |
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| Header | DbId: 8gh DbLabel: GreenFILE An: 184799863 AccessLevel: 6 PubType: Academic Journal PubTypeId: academicJournal PreciseRelevancyScore: 0 |
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| Items | – Name: Title Label: Title Group: Ti Data: Different Faces of the Martian Magnetosphere. – Name: Author Label: Authors Group: Au Data: <searchLink fieldCode="AR" term="%22Dubinin%2C+E%2E%22">Dubinin, E.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> dubinin@mps.mpg.de</i><br /><searchLink fieldCode="AR" term="%22Fraenz%2C+M%2E%22">Fraenz, M.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Modolo%2C+R%2E%22">Modolo, R.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Pätzold%2C+M%2E%22">Pätzold, M.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Tellmann%2C+S%2E%22">Tellmann, S.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22DiBraccio%2C+G%2E%22">DiBraccio, G.</searchLink><relatesTo>4</relatesTo> (AUTHOR) – 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>. Apr2025, Vol. 130 Issue 4, p1-16. 16p. – Name: Subject Label: Subject Terms Group: Su Data: <searchLink fieldCode="DE" term="%22Interplanetary+magnetic+fields%22">Interplanetary magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+magnetic+fields%22">Solar magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetic+dipoles%22">Magnetic dipoles</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetosphere%22">Magnetosphere</searchLink><br /><searchLink fieldCode="DE" term="%22Orbits+%28Astronomy%29%22">Orbits (Astronomy)</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+wind%22">Solar wind</searchLink> – Name: Abstract Label: Abstract Group: Ab Data: The Martian magnetosphere contains components of the induced and intrinsic magnetospheres. Since we can not get a global snapshot of the magnetosphere we use a statistical picture based on a large number of measurements. Depending on the choice of coordinate system and the data selection we can observe different faces of the Martian magnetosphere. If we map data in the Martian Solar Electric coordinate system, then we can separate the induced features of the magnetosphere which appears similar to the magnetosphere of Venus. If we use the Martian Solar Orbital coordinate system and select together the orbits with positive and negative By ${B}_{y}$‐component of the IMF, then the effects related to draped magnetic field and the high order harmonics of the crustal magnetic field are significantly weakened because of averaging over many orbits and a dipole‐like magnetosphere of Mars becomes visible. If we select separately the orbits with positive and negative By ${B}_{y}$‐component we observe a twist of the magnetotail in the direction determined by the sign of By ${B}_{y}$ that is typical for a hybrid magnetosphere with the induced and intrinsic components. The intrinsic and induced components are also well separated when we select the orbits with northward IMF. Then we observe the features that are somewhat similar to those at the Earth magnetosphere. When we use the MSO coordinates and separate by the phase of Mars rotation, the tail topology occurs more complex. This indicates that the effects of the local crustal magnetic field turn out as being also important. Plain Language Summary: The Martian magnetosphere contains features typical for induced and intrinsic magnetospheres. To describe these features we use a picture based on a statistical approach with a large number of measurements. It was shown that utilizing different coordinate systems and selecting orbits with different cross‐flow components of the interplanetary magnetic field in the solar wind we can separate the induced and intrinsic components inherent to the Martian magnetosphere. We can isolate the induced component and observe the features that are in many ways similar to those we see at Venus. Isolating the intrinsic component we have found a dipole‐like obstacle for solar wind. Key Points: The Martian ionosphere contains components of the induced and intrinsic magnetospheresUsing different coordinate systems and averaging on the different data set we can separate these componentsA dipole‐like obstacle for solar wind is revealed [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.) |
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| RecordInfo | BibRecord: BibEntity: Identifiers: – Type: doi Value: 10.1029/2025JA033717 Languages: – Code: eng Text: English PhysicalDescription: Pagination: PageCount: 16 StartPage: 1 Subjects: – SubjectFull: Interplanetary magnetic fields Type: general – SubjectFull: Solar magnetic fields Type: general – SubjectFull: Magnetic dipoles Type: general – SubjectFull: Magnetosphere Type: general – SubjectFull: Orbits (Astronomy) Type: general – SubjectFull: Solar wind Type: general Titles: – TitleFull: Different Faces of the Martian Magnetosphere. Type: main BibRelationships: HasContributorRelationships: – PersonEntity: Name: NameFull: Dubinin, E. – PersonEntity: Name: NameFull: Fraenz, M. – PersonEntity: Name: NameFull: Modolo, R. – PersonEntity: Name: NameFull: Pätzold, M. – PersonEntity: Name: NameFull: Tellmann, S. – PersonEntity: Name: NameFull: DiBraccio, G. IsPartOfRelationships: – BibEntity: Dates: – D: 01 M: 04 Text: Apr2025 Type: published Y: 2025 Identifiers: – Type: issn-print Value: 21699380 Numbering: – Type: volume Value: 130 – Type: issue Value: 4 Titles: – TitleFull: Journal of Geophysical Research. Space Physics Type: main |
| ResultId | 1 |
