Chinese Science Bulletin, Volume 65 , Issue 14 : 1305-1319(2020) https://doi.org/10.1360/TB-2019-0804

Remote sensing of planetary space environment

Fei He 1,2,3,4,*
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  • ReceivedDec 9, 2019
  • AcceptedMar 17, 2020
  • PublishedMar 31, 2020


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感谢中国科学院地质与地球物理研究所尧中华博士对本文的宝贵建议. 感谢中国科学院地质与地球物理研究所魏勇博士提供图2. “风云三号”广角极光成像仪图像数据来源于国家卫星气象中心. “嫦娥三号”极紫外相机数据来源于中国科学院国家天文台探月工程地面应用系统.


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  • Figure 1

    Three typical methods of optical remote sensing. (a) Imaging; (b) spectrograph; (c) spectrographic imaging

  • Figure 2

    Shapes of ionosphere at Venus under different solar wind conditions. (a) Normal ionosphere; (b) tear-dropped ionosphere. Source: Dr. Yong Wei

  • Figure 3

    Side view of the Earth’s plasmasphere imaged by the Extreme Ultraviolet Camera onboard the Chang’E-3 lunar lander. The Earth’s size is marked by the white circle and the Sun is denoted by the filled yellow circle. Typical structures in the image are marked by white arrows

  • Figure 4

    Far ultraviolet auroral image observed by the wide-field auroral imager onboard the Fengyun-3D satellite. The coordinate system is magnetic latitude and magnetic local time

  • Table 1   Parameters of planetary magnetosphere[25]



















    半径, RP(km)

























    表面磁场, B0(nT)









    太阳风密度, ρ(cm−3)








































    10~100 d

    30 d~a

    1~30 d










    1 AU=1.5×108 km; b) 参考美国宇航局行星情况说明书: https://nssdc.gsfc.nasa.gov/planetary/planetfact.html; c) 以地球磁矩归一化, MEarth=7.906×1015 T m3; d) 磁层顶鼻点距离RMP = (B02/2μ0ρu2)1/6/RP, 采用表中典型太阳风密度和太阳风速度u ~ 400 km s−1计算, 对于外行星, 该计算值偏低; e) 等离子体层顶[15]内主要来自电离层, 主要受地球共转电场控制, 时间尺度为天量级, 等离子体顶外主要来自太阳风, 主要受太阳风对流电场控制, 时间尺度为小时量级; f) 土卫二: Enceladus, 土卫三: Tethys, 土卫四: Dione; g) 海卫一: Triton; h) “—”代表该行星不存在此项或无相关测量结果


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