太阳耀斑对热层–电离层–磁层耦合系统影响研究进展

刘宣青; 陈耀; 乐会军; 刘晶

doi:10.11728/cjss2026.05.2025-0218

太阳耀斑对热层–电离层–磁层耦合系统影响研究进展

doi: 10.11728/cjss2026.05.2025-0218 cstr: 32142.14.cjss.2025-0218

刘宣青^1,,
陈耀¹,
乐会军^{2, 3, 4},
刘晶^1, ,

1.
山东大学空间科学与技术学院空间科学研究院山东省太空环境与探测技术重点实验室　威海　264209
2.
中国科学院地质与地球物理研究所行星科学与前沿技术重点实验室　北京　100029
3.
中国科学院大学地球与行星科学学院　北京　100049
4.
中国科学院地质与地球物理研究所黑龙江漠河地球物理国家野外科学观测研究站　北京　100029

基金项目: 国家自然科学基金青年科学基金项目C类 (42604219), 山东省自然科学基金项目 (ZR2022JQ18), 中国博士后科学基金项目 (2025M780366) 和山东省博士后科学基金项目 (SDZZ-ZR-202501257) 共同资助

详细信息

作者简介:

刘宣青　女, 1996年12月出生于山西省朔州市, 现为山东大学空间科学与技术学院博士后, 主要研究方向为太阳耀斑对地球电离层–热层耦合系统影响. E-mail: xuanqingliu@sdu.edu.cn

通讯作者:

刘晶　男, 1983年12月出生于湖北省黄冈市, 现为山东大学空间科学与技术学院教授, 博士生导师, 主要研究方向为地球电离层–磁层耦合系统以及数值与人工智能建模等. E-mail: liujing2019@sdu.edu.cn

中图分类号: P353.7
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出版历程
- 收稿日期: 2025-12-15
- 修回日期: 2026-04-22
- 网络出版日期: 2026-05-08

Research Progress on the Effects of Solar Flares on the Thermosphere-Ionosphere-Magnetosphere (T-I-M) Coupling System

LIU Xuanqing^1
,,
CHEN Yao¹,
LE Huijun^{2, 3, 4},
LIU Jing^{1
, ,}

1.
Shandong Key Laboratory of Space Environment and Exploration Technology, Institute of Space Sciences, School of Space Science and Technology, Shandong University, Weihai 264209
2.
Key Laboratory of Planetary Science and Frontier Technology, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029
3.
College of Earth and Planetary Sciences, University of Chinese Academy of Sciences, Beijing 100049
4.
Heilongjiang Mohe National Observatory of Geophysics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029

摘要

摘要: 作为太阳爆发的重要形式, 耀斑可瞬时释放出强烈的电磁辐射, 可显著扰动地球热层–电离层–磁层(T-I-M)耦合系统. 系统综述了近10年来中国在耀斑对T-I-M(Thermosphere-Ionosphere-Magnetosphere)系统多尺度影响及其耦合物理机制方面的研究进展. 在热层响应方面, 重点总结耀斑引起的热层加热、中性成分变化及大气动力学过程; 在电离层扰动方面, 分析耀斑引发的瞬时光电离响应、动力学变化以及电动力学过程中电场、电流体系的重构, 尤其关注了耀斑极紫外后相对电离层的影响; 在磁层耦合方面, 阐述耀斑通过极区电导率变化调制场向电流与磁层对流结构的观测证据与机理, 探讨耀斑与磁暴共同作用下的非线性耦合特征.
- 太阳耀斑 /
- 热层–电离层–磁层耦合 /
- 空间天气 /
- 极紫外后相
Abstract: Solar flares release intense electromagnetic radiation and can strongly perturb the Earth’s Thermosphere-Ionosphere-Magnetosphere (T-I-M) coupling system. Here, we review progress made by Chinese researchers over the past decade in understanding the multiscale effects of solar flares on the T-I-M system and the underlying coupling mechanisms. For the thermosphere, we summarize flare-induced heating, changes in neutral composition, and atmospheric dynamics. For the ionosphere, we discuss the rapid photoionization response, dynamical changes, and the electrodynamic restructuring of electric fields and current systems, with particular attention to the effects of the extreme ultraviolet late phase. For magnetospheric coupling, we review observational evidence and physical mechanisms showing how flare-driven changes in polar ionospheric conductance modulate field-aligned currents and magnetospheric convection. We also discuss the nonlinear coupling between solar flares and geomagnetic storms.
- Solar flares /
- Thermosphere-Ionosphere-Magnetosphere (T-I-M) coupling /
- Space weather /
- Extreme ultraviolet late phase
注释:
医学伦理:
1) 研究不涉及人体或动物实验.
利益冲突:
2) 所有作者均声明不存在利益冲突.

HTML全文

图 1 距太阳1 AU不同波段的太阳光谱辐射^[25]

Figure 1. Solar spectrum at different wavelengths at 1 AU from the Sun^[25]

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图 2 2010 年 5 月 5 日 C8.8 级耀斑的软 X 射线演化及传统阶段划分^[40]

Figure 2. Soft X-ray evolution and conventional phase classification of the C8.8 flare on 5 May 2010^[40]

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图 3 2010 年 5 月 5 日 C8.8 级耀斑的多波段辐射演化及 EUV 后相特征^[30]

Figure 3. Multiwavelength irradiance evolution and EUV late-phase signature of the C8.8 flare on 5 May 2010^[30]

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图 4 X17级耀斑期间磁赤道正午热层和电离层的模拟响应. (a) 中性温度, (b) 电子密度, (c) 5～105 nm积分EUV^[18]

Figure 4. Simulated thermospheric and ionospheric responses to an X17 flare at the magnetic equator and local noon. (a) Neutral temperature, (b) electron density, (c) integrated EUV at 5-105 nm^[18]

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图 5 TIEGCM模拟的有无耀斑条件下O/N₂差值

Figure 5. TIEGCM-simulated O/N₂ differences between flare and no-flare conditions

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图 6 耀斑发生后400 km高度水平风和中性密度变化

Figure 6. Changes in horizontal wind and neutral density at 400 km after solar flare onset

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图 7 TIME-GCM模拟的2017年9月6－11日热层中性密度(400 km高度). (a) 12:00 LT有耀斑情况, (b) 21:00 LT有耀斑情况, (c) 12:00 LT无耀斑情况, (d) 21:00 LT 无耀斑情况^[18]

Figure 7. TIME‐GCM simulated thermosphere mass density at 400 km from 6 to 11 September 2017. (a) With flares at 12:00 LT, (b) with flares at 21:00 LT, (c) without flares at 12:00 LT, (d) without flares at 21:00 LT^[18]

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图 8 2017年9月6日X9.3级耀斑前及峰值期间全球VTEC, ΔVTEC和EUV变化^[63]

Figure 8. Global VTEC, ΔVTEC, and EUV variations before and during the peak of the X9.3 flare on 6 September 2017^[63]

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图 9 耀斑峰值时北半球不同压力面电子密度差值(耀斑−无耀斑)^[64]

Figure 9. Electron density differences between flare and no-flare conditions at different pressure levels in the Northern Hemisphere at the flare peak^[64]

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图 10 2017年9月6日约40°N处耀斑后TID的纬向传播^[65]

Figure 10. Zonal propagation of postflare TIDs near 40°N on 6 September 2017^[65]

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图 11 模拟的离子垂直速度及不同输运过程的贡献随高度和时间变化. (a) 离子垂直速度 (V_o), (b) 双极扩散 (V_d), (c) 漂移贡献 ($ {V}_{\boldsymbol{E}×\boldsymbol{B}} $), (d) 中性风贡献 ($ {V}_{\text{w}} $)^[66]

Figure 11. Simulated ion vertical velocity and contributions from different transport processes as functions of altitude and UT. (a) Ion vertical geometric velocity (V_o), (b) ambipolar diffusion contributions (V_d), (c) drift contributions ($ {V}_{\boldsymbol{E}\times \boldsymbol{B}} $), (d) neutral winds contributions (V_w)^[66]

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图 12 LTR和TIEGCM模拟的高纬Pedersen电导率和电势分布^[76]

Figure 12. High-latitude Pedersen conductance and electric potential simulated by LTR and TIEGCM^[76]

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图 13 中国不同纬度台站在平静日和耀斑日的电子密度剖面变化^[31]

Figure 13. Electron density profile variations at different latitudes over China on a quiet day and a flare day^[31]

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图 14 全球电离层等效电流在包含ELP的耀斑期间变化情况^[81]

Figure 14. Variation of Sq currents during the solar flare including the EUV late phase^[81]

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图 15 Blackstone雷达对2015年5月15日太阳耀斑的响应. (a) 视场多普勒速度, (b) 波束7的后向散射功率和多普勒速度^[86]

Figure 15. Response of the Blackstone radar to the solar flare on 15 May 2015. (a) FoV Doppler velocity, (b) backscattered power and Doppler velocity on beam 7^[86]

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图 16 2017年9月6日耀斑前后北半球场向电流和Pedersen电导率的观测与模拟结果^[4]

Figure 16. Observed and simulated Northern Hemisphere FACs and Pedersen conductance before and during the flare on 6 September 2017^[4]

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图 17 LTR模拟的2017年9月6日耀斑效应. (a)～(c) 磁层赤道面对流速度, (d)～(f) 高纬电势^[4]

Figure 17. LTR-simulated solar flare effects on 6 September 2017. (a)-(c) Magnetospheric convection velocity in the equatorial plane, (d) - (f) high-latitude electric potential^[4]

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图 18 无磁暴和磁暴条件下LTR模拟的北半球约300 km电子密度和离子对流. (a) (d) 有耀斑, (b) (e) 无耀斑, (c) (f) 两者差值^[87]

Figure 18. LTR-simulated electron density and ion convection at ～300 km in the Northern Hemisphere under nonstorm and storm conditions. (a) (d) With flare, (b) (e) without flare, and (c) (f) their differences^[87]

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太阳耀斑对热层–电离层–磁层耦合系统影响研究进展

doi: 10.11728/cjss2026.05.2025-0218 cstr: 32142.14.cjss.2025-0218

作者简介:

刘宣青　女, 1996年12月出生于山西省朔州市, 现为山东大学空间科学与技术学院博士后, 主要研究方向为太阳耀斑对地球电离层–热层耦合系统影响. E-mail: xuanqingliu@sdu.edu.cn

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刘晶　男, 1983年12月出生于湖北省黄冈市, 现为山东大学空间科学与技术学院教授, 博士生导师, 主要研究方向为地球电离层–磁层耦合系统以及数值与人工智能建模等. E-mail: liujing2019@sdu.edu.cn

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Research Progress on the Effects of Solar Flares on the Thermosphere-Ionosphere-Magnetosphere (T-I-M) Coupling System

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太阳耀斑对热层–电离层–磁层耦合系统影响研究进展

doi: 10.11728/cjss2026.05.2025-0218 cstr: 32142.14.cjss.2025-0218

作者简介: 刘宣青 女, 1996年12月出生于山西省朔州市, 现为山东大学空间科学与技术学院博士后, 主要研究方向为太阳耀斑对地球电离层–热层耦合系统影响. E-mail: xuanqingliu@sdu.edu.cn

通讯作者: 刘晶 男, 1983年12月出生于湖北省黄冈市, 现为山东大学空间科学与技术学院教授, 博士生导师, 主要研究方向为地球电离层–磁层耦合系统以及数值与人工智能建模等. E-mail: liujing2019@sdu.edu.cn

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Research Progress on the Effects of Solar Flares on the Thermosphere-Ionosphere-Magnetosphere (T-I-M) Coupling System

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出版历程

目录

作者简介:

刘宣青　女, 1996年12月出生于山西省朔州市, 现为山东大学空间科学与技术学院博士后, 主要研究方向为太阳耀斑对地球电离层–热层耦合系统影响. E-mail: xuanqingliu@sdu.edu.cn

通讯作者:

刘晶　男, 1983年12月出生于湖北省黄冈市, 现为山东大学空间科学与技术学院教授, 博士生导师, 主要研究方向为地球电离层–磁层耦合系统以及数值与人工智能建模等. E-mail: liujing2019@sdu.edu.cn