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The Influence of Magnetic Topology on Ionospheric Structure at Mars: Observations of Localized 'Magnetic Depletions'.

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Title: The Influence of Magnetic Topology on Ionospheric Structure at Mars: Observations of Localized 'Magnetic Depletions'.
Authors: Fowler, C. M.1 (AUTHOR) christopher.fowler@mail.wvu.edu, Ortiz, J. Z.2 (AUTHOR), Xu, S.2 (AUTHOR), Mitchell, D.2 (AUTHOR), Hanley, K. G.2 (AUTHOR), Espley, J.3 (AUTHOR), Andersson, L.4 (AUTHOR), McFadden, J.2 (AUTHOR), Luhmann, J.2 (AUTHOR), Curry, S.2 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Nov2022, Vol. 127 Issue 11, p1-18. 18p.
Subject Terms: Solar wind, Interplanetary magnetic fields, Martian atmosphere, Solar magnetic fields, Mars (Planet), Magnetic flux density, Solar system
Abstract: The interaction between Mars' crustal magnetic fields and the solar wind produces a variety of magnetic topologies whose characteristics depend upon the plasma regions that the magnetic field is embedded in. We utilize in‐situ Mars Atmosphere And Volatile EvolutioN (MAVEN) measurements to identify localized ionospheric structures, observed as the spacecraft flies through this patchwork of different magnetic topologies. Events are characterized by sharp 'drop outs' in magnetic field strength that we term 'magnetic depletions'. The plasma pressure dominates within magnetic depletions, while the magnetic pressure typically dominates outside of them. Abrupt changes in magnetic topology are coincident with the depletion boundaries. A preliminary statistical study spanning 3 months shows that events occur on ∼4% of MAVEN orbits, between altitudes of 170–360 km. Ionospheric electrons are collisionless and thus magnetized at these altitudes, and combined with the fact that magnetic diffusion timescales range from minutes to an hour, these characteristics suggest that such structures can be observed sporadically by MAVEN on its ∼4.5 hr orbit before being smeared out by magnetic diffusion. At lower altitudes high collision rates lead to diffusion timescales of seconds, while at higher altitudes electromagnetic waves, instabilities and other transport processes driven by the Mars‐solar wind interaction can distort the magnetic field, making magnetic depletion events difficult to identify. Magnetic depletions highlight the ability of magnetic topology to drive localized ionospheric structure at Mars, a result that stems from the unique interaction between the solar wind, Mars' crustal magnetic fields, and it's ionosphere. Plain Language Summary: Our Sun continuously emits a stream of energetic charged particles that travel radially outward across our solar system. This flow of particles, called the solar wind, carries with it a magnetic field that is known as the Interplanetary Magnetic Field. As the solar wind and this magnetic field encounter planets, comets and other bodies within the solar system, a variety of physical processes determine how the solar wind flow is diverted around these bodies, much like water flowing around a rock in a stream. At Mars, magnetic and electric fields play crucial roles in the diversion of this flow. We have used spacecraft observations at Mars to investigate how magnetic fields in particular can produce unique structures within the Mars atmosphere, as a direct result of this interaction between the solar wind flow and the planet. We find that atmospheric conditions are different within these structures, such that a "patchwork" of different conditions can be observed as the spacecraft flies through the Martian atmosphere. Understanding how the solar wind interacts with Mars provides crucial context for understanding how the solar wind interacts with other planets and bodies in our solar system. Key Points: We investigate localized plasma structures in the Mars ionosphere, identified by steep gradients in magnetic field strength'Magnetic depletion' events are observed on a few percent of orbits, between altitudes of 170–360 kmThe complex and variable magnetic topology at Mars appears to drive the formation of these events [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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  Data: The Influence of Magnetic Topology on Ionospheric Structure at Mars: Observations of Localized 'Magnetic Depletions'.
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  Data: <searchLink fieldCode="AR" term="%22Fowler%2C+C%2E+M%2E%22">Fowler, C. M.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> christopher.fowler@mail.wvu.edu</i><br /><searchLink fieldCode="AR" term="%22Ortiz%2C+J%2E+Z%2E%22">Ortiz, J. Z.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Xu%2C+S%2E%22">Xu, S.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Mitchell%2C+D%2E%22">Mitchell, D.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Hanley%2C+K%2E+G%2E%22">Hanley, K. G.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Espley%2C+J%2E%22">Espley, J.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Andersson%2C+L%2E%22">Andersson, L.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22McFadden%2C+J%2E%22">McFadden, J.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Luhmann%2C+J%2E%22">Luhmann, J.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Curry%2C+S%2E%22">Curry, S.</searchLink><relatesTo>2</relatesTo> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Space+Physics%22">Journal of Geophysical Research. Space Physics</searchLink>. Nov2022, Vol. 127 Issue 11, p1-18. 18p.
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  Data: <searchLink fieldCode="DE" term="%22Solar+wind%22">Solar wind</searchLink><br /><searchLink fieldCode="DE" term="%22Interplanetary+magnetic+fields%22">Interplanetary magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Martian+atmosphere%22">Martian atmosphere</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+magnetic+fields%22">Solar magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Mars+%28Planet%29%22">Mars (Planet)</searchLink><br /><searchLink fieldCode="DE" term="%22Magnetic+flux+density%22">Magnetic flux density</searchLink><br /><searchLink fieldCode="DE" term="%22Solar+system%22">Solar system</searchLink>
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  Data: The interaction between Mars' crustal magnetic fields and the solar wind produces a variety of magnetic topologies whose characteristics depend upon the plasma regions that the magnetic field is embedded in. We utilize in‐situ Mars Atmosphere And Volatile EvolutioN (MAVEN) measurements to identify localized ionospheric structures, observed as the spacecraft flies through this patchwork of different magnetic topologies. Events are characterized by sharp 'drop outs' in magnetic field strength that we term 'magnetic depletions'. The plasma pressure dominates within magnetic depletions, while the magnetic pressure typically dominates outside of them. Abrupt changes in magnetic topology are coincident with the depletion boundaries. A preliminary statistical study spanning 3 months shows that events occur on ∼4% of MAVEN orbits, between altitudes of 170–360 km. Ionospheric electrons are collisionless and thus magnetized at these altitudes, and combined with the fact that magnetic diffusion timescales range from minutes to an hour, these characteristics suggest that such structures can be observed sporadically by MAVEN on its ∼4.5 hr orbit before being smeared out by magnetic diffusion. At lower altitudes high collision rates lead to diffusion timescales of seconds, while at higher altitudes electromagnetic waves, instabilities and other transport processes driven by the Mars‐solar wind interaction can distort the magnetic field, making magnetic depletion events difficult to identify. Magnetic depletions highlight the ability of magnetic topology to drive localized ionospheric structure at Mars, a result that stems from the unique interaction between the solar wind, Mars' crustal magnetic fields, and it's ionosphere. Plain Language Summary: Our Sun continuously emits a stream of energetic charged particles that travel radially outward across our solar system. This flow of particles, called the solar wind, carries with it a magnetic field that is known as the Interplanetary Magnetic Field. As the solar wind and this magnetic field encounter planets, comets and other bodies within the solar system, a variety of physical processes determine how the solar wind flow is diverted around these bodies, much like water flowing around a rock in a stream. At Mars, magnetic and electric fields play crucial roles in the diversion of this flow. We have used spacecraft observations at Mars to investigate how magnetic fields in particular can produce unique structures within the Mars atmosphere, as a direct result of this interaction between the solar wind flow and the planet. We find that atmospheric conditions are different within these structures, such that a "patchwork" of different conditions can be observed as the spacecraft flies through the Martian atmosphere. Understanding how the solar wind interacts with Mars provides crucial context for understanding how the solar wind interacts with other planets and bodies in our solar system. Key Points: We investigate localized plasma structures in the Mars ionosphere, identified by steep gradients in magnetic field strength'Magnetic depletion' events are observed on a few percent of orbits, between altitudes of 170–360 kmThe complex and variable magnetic topology at Mars appears to drive the formation of these events [ABSTRACT FROM AUTHOR]
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  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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        Value: 10.1029/2022JA030727
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      – Code: eng
        Text: English
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      – SubjectFull: Interplanetary magnetic fields
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      – SubjectFull: Martian atmosphere
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      – SubjectFull: Solar magnetic fields
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      – SubjectFull: Mars (Planet)
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      – SubjectFull: Magnetic flux density
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      – SubjectFull: Solar system
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      – TitleFull: The Influence of Magnetic Topology on Ionospheric Structure at Mars: Observations of Localized 'Magnetic Depletions'.
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              Text: Nov2022
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