A Simulation Study of Martian Airglow Emission Response to the X8.2 Solar Flare on 10 September 2017

IF 3.9 1区地球科学 Q1 GEOCHEMISTRY & GEOPHYSICS

Journal of Geophysical Research: Planets Pub Date : 2025-05-15 DOI:10.1029/2024JE008878

Zerui Liu, Jiuhou Lei, Maodong Yan, Tong Dang

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引用次数: 0

Abstract

During the solar flare, the planetary upper atmosphere and ionosphere are rapidly impacted, and the airglow emission intensity can be significantly enhanced. Previous studies have been carried out on the variation of Martian airglow emissions using the Imaging Ultraviolet Spectrograph instrument aboard the Mars Atmosphere Volatile EvolutioN mission. However, the underlying mechanisms responsible for Martian emission intensity during solar flare events remain to be addressed. In this study, we explore the variation of the emission intensity caused by the X8.2 solar flare on 10 September 2017, using photoelectron transport model, focusing on two typical emission spectra— ${CO}_{2}^{+}$ Ultraviolet doublet (UVD) and $CO$ Cameron band. We show the comparison of the simulated and observed emission intensity and find that the variation trend with altitude of simulated limb intensity is in agreement with the observation. In both the simulated and observed results, a sub-peak in the limb intensity around 100 km is observed, attributed to the photoelectron impact process. Additionally, the photoelectron impact process responds more strongly to the solar flare than the photon impact process, and leads to a sharper sub-peak at the peak flare period. Furthermore, the photon impact process, causing the different response of ${CO}_{2}^{+} (B^{2} Σ_{u}^{+})$ and $CO (a^{3} Π)$ to solar flares, is linked to the distinct value domains of the photon impact cross sections throughout the spectral band.

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2017年9月10日X8.2太阳耀斑对火星气辉辐射响应的模拟研究

在太阳耀斑期间，行星上层大气和电离层受到快速冲击，气辉发射强度显著增强。以前的研究是利用火星大气挥发性演化任务上的成像紫外光谱仪对火星气辉发射的变化进行的。然而，在太阳耀斑事件期间负责火星发射强度的潜在机制仍有待解决。在本研究中，我们利用光电子输运模型，探讨了2017年9月10日X8.2太阳耀斑引起的发射强度变化。重点研究了两种典型的发射光谱——co2 + ${\text{CO}}_{2}^{+}$紫外双峰（UVD）和CO $\text{CO}$ Cameron波段。将模拟的辐射强度与观测的辐射强度进行比较，发现模拟辐射强度随海拔的变化趋势与观测结果一致。在模拟和观测结果中，在100 km左右观察到一个分支强度的次峰，这归因于光电子撞击过程。此外，光电子冲击过程对太阳耀斑的响应比光子冲击过程更强烈，并且在耀斑高峰期产生一个更尖锐的子峰。此外，光子撞击过程，造成co2 + b2 Σ u +的不同反应${\text{CO}}_{2}^{+}\left({\mathrm{B}}^{2}{{\Sigma }}_{\mathrm{u}}^{+}\right)$和coa3 Π $\text{CO}\left({\mathrm{a}}^{3}{\Pi }\right)$到太阳耀斑，与整个光谱带中光子撞击截面的不同值域有关。

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来源期刊

Journal of Geophysical Research: Planets Earth and Planetary Sciences-Earth and Planetary Sciences (miscellaneous)

CiteScore

8.00

自引率

27.10%

发文量

254

期刊介绍： The Journal of Geophysical Research Planets is dedicated to the publication of new and original research in the broad field of planetary science. Manuscripts concerning planetary geology, geophysics, geochemistry, atmospheres, and dynamics are appropriate for the journal when they increase knowledge about the processes that affect Solar System objects. Manuscripts concerning other planetary systems, exoplanets or Earth are welcome when presented in a comparative planetology perspective. Studies in the field of astrobiology will be considered when they have immediate consequences for the interpretation of planetary data. JGR: Planets does not publish manuscripts that deal with future missions and instrumentation, nor those that are primarily of an engineering interest. Instrument, calibration or data processing papers may be appropriate for the journal, but only when accompanied by scientific analysis and interpretation that increases understanding of the studied object. A manuscript that describes a new method or technique would be acceptable for JGR: Planets if it contained new and relevant scientific results obtained using the method. Review articles are generally not appropriate for JGR: Planets, but they may be considered if they form an integral part of a special issue.