Volume 44 Issue 2
Apr.  2024
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ZHANG Yiteng, LI Lei, XIE Lianghai, GOU Xiaochen, FENG Yongyong. Distribution and Characteristics of Martian Precipitating H-ENA (in Chinese). Chinese Journal of Space Science, 2024, 44(2): 299-308 doi: 10.11728/cjss2024.02.2023-0044
Citation: ZHANG Yiteng, LI Lei, XIE Lianghai, GOU Xiaochen, FENG Yongyong. Distribution and Characteristics of Martian Precipitating H-ENA (in Chinese). Chinese Journal of Space Science, 2024, 44(2): 299-308 doi: 10.11728/cjss2024.02.2023-0044
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Distribution and Characteristics of Martian Precipitating H-ENA

doi: 10.11728/cjss2024.02.2023-0044 cstr: 32142.14.cjss2024.02.2023-0044
  • 1.

    State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190

  • 2.

    University of Chinese Academy of Sciences, Beijing 100049

  • 3.

    National Space Science Center, Chinese Academy of Sciences, Beijing 100190

  • 4.

    Joint Research and Development Center of Chinese Science Academy and Shen County, Liaocheng 252400

  • Received Date: 2023-04-07
  • Rev Recd Date: 2023-04-20
    • Available Online: 2023-12-15
    Abstract
  • Energetic Neutral Atom (ENA) is generated by charge exchange between energetic ions and background neutrals. As Martian exosphere extends far above the bow shock, hydrogen ENA (H-ENA) produced by solar wind proton may enter the lower atmosphere directly, depositing mass and energy in the atmosphere. Based on the single-fluid multispecies MHD model and exosphere model, this paper calculates the spatial distribution of the precipitating H-ENA flux at the height of 200 km on Mars, evaluates the particle and energy deposition rate of the precipitating H-ENA under different solar wind conditions, analyzes their controlling factors. The results show that the solar wind H-ENA generated upstream of the bow shock is less affected by the crustal fields, and shows a cosZ distribution. As a major mass and energy source, the precipitating solar wind H-ENAs account for 59% particle deposition and 81% energy deposition of the total precipitating ENAs. Magnetosheath H-ENA generated in the magnetosheath is greatly affected by the crustal fields, and their precipitating flux decreases significantly above the strongest magnetic anomalies. The precipitating H-ENA flux is proportional to the upstream solar wind flux, and 2.1%～3.5% of upstream solar wind protons are estimated to be converted into the solar wind H-ENAs.

     

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