In‐Situ Measurements of Electron Temperature and Density in Mars' Dayside Ionosphere

Ergun, R. E.; Andersson, L.; Fowler, C. M.; Thaller, S. A.; Yelle, R. V.

doi:10.1029/2021gl093623

Cited by 21 publications

(21 citation statements)

References 36 publications

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“…The even larger discrepancy between electron and neutral temperatures is discussed in detail by Ergun, Andersson, Fowler, Thaller, et al. ( 2021 ). We begin with photoionization, which produces radicals that participate in a network of chemical reactions.…”

Section: Discussionmentioning

confidence: 87%

In Situ Measurements of Thermal Ion Temperature in the Martian Ionosphere

et al. 2021

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Ion temperature is an important parameter that influences the structure and evolution of atmospheres (Schunk & Nagy, 2009). Ion temperatures affect collision and chemical reaction rates, so precise knowledge of ion temperatures and the chemical processes operating in planetary atmospheres enables a more thorough understanding of composition and structure in the photochemical region (Fox, 2015). Ion temperatures also influence atmospheric dynamics and energetics. Specifically, hotter temperatures allow more ions to overcome gravity and reach altitudes above the exobase, where electromagnetic forces can accelerate ions to escape velocity. Understanding how ions are supplied to the exosphere is important for a complete description of ion escape during the present epoch (Chassefière & Leblanc, 2004), and can illuminate how ion loss might have varied under different conditions at

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Section: Discussionmentioning

confidence: 87%

In Situ Measurements of Thermal Ion Temperature in the Martian Ionosphere

et al. 2021

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“…The uncertainty in k 4 might be improved with the new calibrated LPW electron temperature reported in Ergun et al. (2021), however, those data have not been published yet.…”

Section: Discussionmentioning

confidence: 95%

“…The small variation in O 2 + density in the PCE model might be the uncertainty in the dissociative recombination rate of k 4 and the effects of dynamics (Fox, 2009). The uncertainty in k 4 might be improved with the new calibrated LPW electron temperature reported in Ergun et al (2021), however, those data have not been published yet.…”

Section: Seasonal Variation In Ion Density Under the Pcementioning

confidence: 99%

Seasonal and Dust‐Related Variations in the Dayside Thermospheric and Ionospheric Compositions of Mars Observed by MAVEN/NGIMS

et al. 2021

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“…Thermal electron density and temperature are provided by LPW via the analysis of current-voltage curves (Ergun et al, 2015Ergun, Andersson, Fowler, Thaller, & Yelle, 2021). Observations of suprathermal electrons at energies 3 eV-4 keV are provided by SWEA, an electrostatic top hat analyzer.…”

Section: Data Setsmentioning

confidence: 99%

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

et al. 2022

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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 trueV⃗×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.

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In‐Situ Measurements of Electron Temperature and Density in Mars' Dayside Ionosphere

Cited by 21 publications

References 36 publications

In Situ Measurements of Thermal Ion Temperature in the Martian Ionosphere

In Situ Measurements of Thermal Ion Temperature in the Martian Ionosphere

Seasonal and Dust‐Related Variations in the Dayside Thermospheric and Ionospheric Compositions of Mars Observed by MAVEN/NGIMS

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

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