Effect of the 2018 Martian Global Dust Storm on the Main Species in the Upper Ionosphere: Observations and Simulations

Qin, Jun; Zou, Hong; Lee, Yuni; Ye, Yuguang; Hao, Yongqiang; Wang, Jing-Song

doi:10.1029/2022je007297

Cited by 6 publications

(1 citation statement)

References 35 publications

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“…Bougher et al. (2001) indicated that the Martian dayside ionospheric peak is sensitive to the state of the underlying atmosphere, where dust storm can change the O + and

{\text{CO}}_{2}^{+}

density at ionospheric altitude (Qin, Zou, Lee, et al., 2022). In the absence of these atmospheric processes, the crustal field is the main endogenous source of north‐south asymmetry.…”

Section: Discussionmentioning

confidence: 99%

Effects of Solar Wind Density and Velocity Variations on the Martian Ionosphere and Plasma transport—A MHD Model Study

Song,

Lu,

Cao

et al. 2023

JGR Space Physics

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Solar wind dynamic pressure, consisting solar wind density nsw and velocity Vsw, is an important external driver that controls Martian plasma environment. In this study, a 3D magnetohydrodynamic model is applied to investigate the separate influences of solar wind density and velocity on the Martian ionosphere. The spatial distributions of ions in the dayside and near nightside ionosphere under different nsw and Vsw are analyzed, as well as the ion transport process. We find that for the same dynamic pressure condition, the ionosphere extends to higher altitudes under higher solar wind density, indicating that a solar wind velocity enhancement event is more efficient at compressing the Martian ionosphere. A higher Vsw will result in a stronger induced magnetic field, shielding the Martian ionosphere, preventing the penetration of solar wind particles. For the same dynamic pressure, increasing nsw (decreasing Vsw) leads to a higher horizontal ion velocity, facilitating day‐to‐night plasma transport. As a result, the ionosphere extends farther into the nightside. Also, the ion outflow flux is larger for high nsw, which may lead to a higher escape rate. Moreover, the strong crustal fields in the southern hemisphere also cause significant effect to the ionosphere, hindering horizontal ion transport. An additional outflow channel is also provided by the crustal field on the southern dayside, causing different responses of flow pattern between local and global scale while the solar wind condition is varied.

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“…Bougher et al. (2001) indicated that the Martian dayside ionospheric peak is sensitive to the state of the underlying atmosphere, where dust storm can change the O + and

{\text{CO}}_{2}^{+}

density at ionospheric altitude (Qin, Zou, Lee, et al., 2022). In the absence of these atmospheric processes, the crustal field is the main endogenous source of north‐south asymmetry.…”

Section: Discussionmentioning

confidence: 99%