Simulation on the Impact of the Sudden Process of Solar Activity on the Near Space Atmosphere
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摘要: 空间天气对地球及近地空间具有重要影响，大的空间天气事件对中上层大气动力学和成分具有不同的影响。利用全大气耦合模式WACCM，针对太阳耀斑、太阳质子、地磁暴三类事件，以太阳活动平静期2015年5月10－14日的GEOS-5数据为模式背景场，通过F10.7、离子产生率、Kp及Ap指数设置，分别模拟三类事件对临近空间大气温度、密度和臭氧的影响。结果表明耀斑事件在三类事件中对临近空间大气温度和密度的影响最为显著。平流层大气温度增加是由耀斑辐射增强引起平流层臭氧吸收紫外辐射发生的光化学反应所致，耀斑事件引起平流层和低热层温度增加约为2~3 K，低热层大气相对密度增加在6%以内；太阳质子事件及磁暴事件主要影响低热层，但太阳质子事件和磁暴事件对低热层温度扰动不大于1 K。Abstract: Space weather has important effects on the Earth and near-Earth space, while large space weather events have different effects on the dynamics and composition of the pelagic atmosphere. The Whole Atmosphere Community Climate Model (WACCM) is used to simulate the effects of three types of events on atmospheric parameters of high altitude atmospheric parameters in the near space, atmospheric temperature, density and ozone through F10.7, ion production rate, Kp, and Ap index settings, respectively, for solar flares, solar protons and geomagnetic storms. The results show that flare events have the most significant effect on the temperature and density of the near space atmosphere among the three types of events, and the increase in stratospheric atmospheric temperature is caused by the photochemical reaction caused by stratospheric ozone absorption of ultraviolet radiation caused by the enhancement of radiation during the solar flare event, the increase of temperature in stratosphere and low thermosphere is roughly 2~3 K, and the relative density of the lower thermosphere increases within 6%. Solar proton events and geomagnetic storm events mainly affect the low thermosphere, but solar proton events and magnetic storm events disturb the temperature of the lower thermosphere by no more than 1 K.
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Key words:
- Solar activity /
- Near space /
- Modeling /
- Response characteristics
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图 4 2015年5月12日离子产生率随气压的变化
Figure 4. Solar proton event ion production rates as a function of pressure on 12 May 2015
图 5 三种事件中20°N温度改变量随时间–高度变化
Figure 5. Time-altitude evolution of temperature changes between the experimental simulation and the baseline simulation in 20°N of three types of events
图 6 三种事件中40°N温度改变量随时间–高度的变化
Figure 6. Time-altitude evolution of temperature changes between the experimental simulation and the baseline simulation in 40°N of three types of events
图 7 三种事件中70°N温度改变量随时间–高度的变化
Figure 7. Time-altitude evolution of temperature changes between the experimental simulation and the baseline simulation in 70°N of three types of events
图 8 三种事件中20°N相对密度改变量随时间–高度的变化
Figure 8. Time-altitude evolution of relative density changes between the experimental simulation and the baseline simulation in 20°N of three types of events
图 9 三种事件中40°N相对密度改变量随时间–高度的变化
Figure 9. Time-altitude evolution of relative density changes between the experimental simulation and the baseline simulation in 40°N of three types of events
图 10 三种事件中70°N相对密度改变量随时间–高度的变化
Figure 10. Time-altitude evolution of relative density changes between the experimental simulation and the baseline simulation in 70°N of three types of events
图 11 三种事件中20°N臭氧改变量随时间–高度变化
Figure 11. Time-altitude evolution of ozone changes between the experimental simulation and the baseline simulation in 20°N of three types of events
图 12 三种事件中40°N臭氧改变量随时间–高度变化
Figure 12. Time-altitude evolution of ozone changes between the experimental simulation and the baseline simulation in 40°N of three types of events
图 13 三种事件中70°N臭氧改变量随时间–高度变化
Figure 13. Time-altitude evolution of ozone changes between the experimental simulation and the baseline simulation in 70°N of three types of events
图 14 太阳耀斑事件中20°N，40°N，70°N纬向风随时间–高度的变化
Figure 14. Time-altitude evolution of zonal wind changes between the experimental simulation and the baseline simulation in 20°N, 40°N, 70°N in solar flare event
图 15 太阳耀斑事件中20°N，40°N，70°N经向风随时间–高度的变化
Figure 15. Time-altitude evolution of meridional wind changes between the experimental simulation and the baseline simulation in 20°N, 40°N,70°N in solar flare event
表 1 离子产生率数据来源
Table 1. Introduction of data source of ion production rate
Years Source of Protons 1963－1973 IMP 1～7 1974－1993 IMP 8 1994－2005 GOES 7，8，10，11 2006－2012 GOES 11，13 
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表 2 输入参数设置（模拟时间: 2015年5月10－14日）
Table 2. Input parameter setting (Simulation time: 10 to 14 May 2015)
组别 F10.7 F10.7 a Kp Ap isn IP / (cm–3·s–1) 第一组
太阳耀斑事件190 70 1 3 150 0 第二组
地磁暴事件70 70 7 150 20 0 第三组
太阳质子事件70 70 1 3 20 随气压变化函数，采用真实事件数据输入 第四组
平静对照组70 70 1 3 20 0 注 IP为 Ion Production。
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