Evaluation for effects of variable Martian upper atmosphere on ionospheric peak electron density based on the MGS RO observation

Chen, Yiding; Liu, Libo; Le, Huijun; Zhang, Hui; Zhang, Ruilong

doi:10.1016/j.icarus.2022.115364

Cited by 4 publications

(3 citation statements)

References 53 publications

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“…where SF is the solar ionization radiation flux; its variation can be indicated by the solar 10.7 cm radio flux. The cosine function is a good approximation for describing the N m M 2 variation of the Martian ionosphere even if the SZA is large but not very close to 90°(e.g., Chen et al 2023). The difference in the solar radiation ionization effect is ∼22.5% according to the mean SZAs and SFs of the two profiles, lower than the observed N m M 2 difference of 28%.…”

Section: Resultsmentioning

confidence: 63%

“…In this study, the MGS RO measurements in that longitude region with stronger crustal fields are used to investigate the effect of varying crustal fields on the ionospheric main peak. Ionospheric variation along longitudes is also affected by the upper atmosphere variation related to nonmigrating tides (e.g., Bougher et al 2001;Cahoy et al 2006;Chen et al 2022Chen et al , 2023Fang et al 2021;Haider et al 2006;Krymskii et al 2003;Mahajan et al 2007). Thus, the measurements in the broad longitude region with very weak crustal fields are not included in order to suppress the effect of upper atmosphere variation as far as possible.…”

Section: Datamentioning

confidence: 99%

“…The improved proxy 0.4F 10.7 +0.6F 10.7A (F 10.7A is the 81 day running average of F 10. 7) is used because it can scale the solar ionization radiation variation better than F 10.7 (Chen et al 2012(Chen et al , 2023. It has been normalized from the Sun-Earth distance to the Sun-Mars distance, and the solar longitude difference between the Earth and Mars has been taken into account.…”

Section: Datamentioning

confidence: 99%

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Martian Crustal Magnetic Field Effects on the Ionospheric Main Peak

Chen,

Liu,

et al. 2024

ApJ

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Planetary magnetic fields can affect ionospheric plasma transport and coupling with the solar wind. In contrast to the terrestrial global magnetic field, there are only weaker and sporadic crustal magnetic fields on Mars. Many studies have indicated that Martian crustal fields can still modulate the topside ionosphere and its coupling with the solar wind. Nevertheless, it is unclear whether the crustal fields can affect the ionospheric main peak, which does not directly interact with the solar wind and is dominated by photochemical processes. In this study, the crustal field effect was identified from ionospheric measurements over unevenly distributed crustal fields. Both the intensity and configuration of the crustal fields were found to be capable of affecting the ionospheric main peak. The ionospheric peak electron density tends to decrease in the strong horizontal crustal field region. The results suggest that the crustal fields may affect the ionospheric main peak through modulating solar wind energetic particle precipitation; strong horizontal magnetic fields can partially prevent energetic particle precipitation and thus weaken impact ionization.

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Section: Resultsmentioning

confidence: 63%

Section: Datamentioning

confidence: 99%

Section: Datamentioning

confidence: 99%

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Martian Crustal Magnetic Field Effects on the Ionospheric Main Peak

Chen,

Liu,

et al. 2024

ApJ

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Longitude structure of Martian upper atmosphere seen from MAVEN/NGIMS during 2018 Mars dust storm

Liu,

et al. 2024

Icarus

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A Statistical Study of the Vertical Scale Height of the Martian Ionosphere Using MAVEN Observations

Liu,

Chen

et al. 2024

JGR Planets

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The Vertical Scale Height (VSH) is a crucial parameter that describes the shape of the ionospheric electron density profile. Evidence suggests a complex relationship between VSH and the thermal structure and dynamics of the ionosphere. A statistical study was conducted on the VSH at low altitudes (175 km) and high altitudes (300 km) in the Martian ionosphere, using data from the MAVEN observations from 2014 to 2023. The results suggest that the influence of the crustal magnetic field on VSH175 is more pronounced than on VSH300. VSH175 shows a minor peak around −20° latitudes, which is more than 7% higher than the average value, and an increasing trend with latitude in the northern hemisphere. VSH300 is higher in the southern hemisphere than in the northern hemisphere, especially in summer, by approximately 42.1%. Regarding the local time variation of VSH, we observed an increasing trend from midnight to morning and a decreasing trend from dusk to midnight in almost all conditions. The local time variation of VSH also exhibits seasonal and latitudinal dependence. These variations have different levels of consistency with the gradient of the electron temperature (Te) and the collision frequency between charged particles and neutrals. Specifically, the correlation coefficient between VSH175 and the collision frequency between charged particles and neutrals reaches as high as 0.93 in the northern hemisphere winter and southern hemisphere summer. The correlation coefficient between VSH300 and the gradient of the Te reaches up to 0.72 in the southern hemisphere equinox.

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Evaluation for effects of variable Martian upper atmosphere on ionospheric peak electron density based on the MGS RO observation

Cited by 4 publications

References 53 publications

Martian Crustal Magnetic Field Effects on the Ionospheric Main Peak

Martian Crustal Magnetic Field Effects on the Ionospheric Main Peak

Longitude structure of Martian upper atmosphere seen from MAVEN/NGIMS during 2018 Mars dust storm

A Statistical Study of the Vertical Scale Height of the Martian Ionosphere Using MAVEN Observations

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