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A MAVEN Case Study of Radial IMF at Mars: Impacts on the Dayside Ionosphere.

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Title: A MAVEN Case Study of Radial IMF at Mars: Impacts on the Dayside Ionosphere.
Authors: Fowler, C. M.1 (AUTHOR) christopher.fowler@mail.wvu.edu, Hanley, K. G.2 (AUTHOR), McFadden, J.2 (AUTHOR), Halekas, J.3 (AUTHOR), Schwartz, S. J.4 (AUTHOR), Mazelle, C.5 (AUTHOR), Chaffin, M.4 (AUTHOR), Mitchell, D.2 (AUTHOR), Espley, J.6 (AUTHOR), Ramstad, R.4 (AUTHOR), Dong, Y.4 (AUTHOR), Curry, S.2 (AUTHOR)
Source: Journal of Geophysical Research. Space Physics. Dec2022, Vol. 127 Issue 12, p1-21. 21p.
Subject Terms: *Ionosphere, Solar wind, Interplanetary magnetic fields, Solar magnetic fields, Space environment, Martian atmosphere
Abstract: The solar wind interaction with Mars controls the transfer of energy and momentum from the solar wind into the magnetosphere, ionosphere and atmosphere, driving structure, and dynamics within each. This interaction is highly dependent on the upstream Interplanetary Magnetic Field (IMF) orientation. We use in‐situ plasma measurements made by the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission to identify several prominent features that arise when the IMF is aligned approximately parallel or antiparallel to solar wind flow (conditions known as "radial IMF"). In particular, solar wind protons and alphas are observed to directly penetrate down to periapsis altitudes, while the magnetic barrier forms deep within the dayside ionosphere. The MAVEN observations are consistent with either an ionopause‐like boundary or diamagnetic cavity forming beneath the barrier, as a consequence of the dense cold ionosphere and the absence of significant crustal magnetic fields at this periapsis location. The planetary ions above the magnetic barrier are exposed to solar wind flow and subsequent mass‐loading. The V⃗×B⃗ $\vec{V}\times \vec{B}$ (convective electric field or "ion pickup") force is weak and highly variable during radial IMF. While wave particle interactions and subsequent wave heating contribute to incorporating the heavy planetary ions into the solar wind flow, the solar wind momentum is not fully deflected around the obstacle and is delivered into the collisional atmosphere. Significant ion heating is observed deep within the dayside ionosphere, and observed ionospheric density and temperature profiles demonstrate that these ion energization mechanisms drive significant erosion and likely escape to space. Plain Language Summary: The planets and comets in our solar system are exposed to a barrage of energetic particles emitted by our Sun, known as the solar wind. These particles carry with them a magnetic field, and this magnetic field plays an important role in determining how the solar wind is deflected around these planetary and cometary bodies. We use observations made by a spacecraft orbiting Mars to investigate this interaction when the solar wind magnetic field is oriented in a somewhat unique fashion, aligned in the same direction as the solar wind flow (in contrast to more typical conditions when the solar wind magnetic field is oriented at an angle to the flow direction). In this unique orientation, we find that solar wind particles crash into the dayside atmosphere of Mars, instead of being deflected around the planet. In addition, this magnetic field orientation allows significant solar wind energy to be deposited into the dayside atmosphere via the interaction of generated electric and magnetic fields, with charged particles in the atmosphere. The resulting near space environment at Mars is highly dynamic and disturbed compared to more typical conditions. Key Points: During radial interplanetary magnetic field conditions at Mars, the magnetic barrier forms deep within the dayside ionospherePlanetary ions above the magnetic barrier are exposed to solar wind flow and coupled via weak V⃗×B⃗ $\vec{V}\times \vec{B}$ and strong wave particle interactionsPlasma temperatures are enhanced by factors of 2–10 within the ionosphere; concurrently the dayside ionosphere is significantly eroded [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: A MAVEN Case Study of Radial IMF at Mars: Impacts on the Dayside Ionosphere.
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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="%22Hanley%2C+K%2E+G%2E%22">Hanley, K. G.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22McFadden%2C+J%2E%22">McFadden, J.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Halekas%2C+J%2E%22">Halekas, J.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Schwartz%2C+S%2E+J%2E%22">Schwartz, S. J.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Mazelle%2C+C%2E%22">Mazelle, C.</searchLink><relatesTo>5</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Chaffin%2C+M%2E%22">Chaffin, M.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Mitchell%2C+D%2E%22">Mitchell, D.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Espley%2C+J%2E%22">Espley, J.</searchLink><relatesTo>6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ramstad%2C+R%2E%22">Ramstad, R.</searchLink><relatesTo>4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Dong%2C+Y%2E%22">Dong, Y.</searchLink><relatesTo>4</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>. Dec2022, Vol. 127 Issue 12, p1-21. 21p.
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  Data: *<searchLink fieldCode="DE" term="%22Ionosphere%22">Ionosphere</searchLink><br /><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="%22Solar+magnetic+fields%22">Solar magnetic fields</searchLink><br /><searchLink fieldCode="DE" term="%22Space+environment%22">Space environment</searchLink><br /><searchLink fieldCode="DE" term="%22Martian+atmosphere%22">Martian atmosphere</searchLink>
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  Data: The solar wind interaction with Mars controls the transfer of energy and momentum from the solar wind into the magnetosphere, ionosphere and atmosphere, driving structure, and dynamics within each. This interaction is highly dependent on the upstream Interplanetary Magnetic Field (IMF) orientation. We use in‐situ plasma measurements made by the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission to identify several prominent features that arise when the IMF is aligned approximately parallel or antiparallel to solar wind flow (conditions known as "radial IMF"). In particular, solar wind protons and alphas are observed to directly penetrate down to periapsis altitudes, while the magnetic barrier forms deep within the dayside ionosphere. The MAVEN observations are consistent with either an ionopause‐like boundary or diamagnetic cavity forming beneath the barrier, as a consequence of the dense cold ionosphere and the absence of significant crustal magnetic fields at this periapsis location. The planetary ions above the magnetic barrier are exposed to solar wind flow and subsequent mass‐loading. The V⃗×B⃗ $\vec{V}\times \vec{B}$ (convective electric field or "ion pickup") force is weak and highly variable during radial IMF. While wave particle interactions and subsequent wave heating contribute to incorporating the heavy planetary ions into the solar wind flow, the solar wind momentum is not fully deflected around the obstacle and is delivered into the collisional atmosphere. Significant ion heating is observed deep within the dayside ionosphere, and observed ionospheric density and temperature profiles demonstrate that these ion energization mechanisms drive significant erosion and likely escape to space. Plain Language Summary: The planets and comets in our solar system are exposed to a barrage of energetic particles emitted by our Sun, known as the solar wind. These particles carry with them a magnetic field, and this magnetic field plays an important role in determining how the solar wind is deflected around these planetary and cometary bodies. We use observations made by a spacecraft orbiting Mars to investigate this interaction when the solar wind magnetic field is oriented in a somewhat unique fashion, aligned in the same direction as the solar wind flow (in contrast to more typical conditions when the solar wind magnetic field is oriented at an angle to the flow direction). In this unique orientation, we find that solar wind particles crash into the dayside atmosphere of Mars, instead of being deflected around the planet. In addition, this magnetic field orientation allows significant solar wind energy to be deposited into the dayside atmosphere via the interaction of generated electric and magnetic fields, with charged particles in the atmosphere. The resulting near space environment at Mars is highly dynamic and disturbed compared to more typical conditions. Key Points: During radial interplanetary magnetic field conditions at Mars, the magnetic barrier forms deep within the dayside ionospherePlanetary ions above the magnetic barrier are exposed to solar wind flow and coupled via weak V⃗×B⃗ $\vec{V}\times \vec{B}$ and strong wave particle interactionsPlasma temperatures are enhanced by factors of 2–10 within the ionosphere; concurrently the dayside ionosphere is significantly eroded [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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        Value: 10.1029/2022JA030726
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        Text: English
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        PageCount: 21
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      – SubjectFull: Ionosphere
        Type: general
      – SubjectFull: Solar wind
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      – SubjectFull: Interplanetary magnetic fields
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      – SubjectFull: Space environment
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      – SubjectFull: Martian atmosphere
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