An analysis of thermospheric density response to solar flares during 2001–2006
An analysis of thermospheric density response to solar flares during 2001–2006
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DOI：
10.1029/2011ja017214
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发表时间：
2012-03
影响因子：
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通讯作者：
H. Le;Libo Liu;W. Wan
中科院分区：
文献类型：
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作者：
H. Le;Libo Liu;W. Wan
以往的研究表明，2003年10月28日（X17.2）和2003年11月4日（X28）的两次大耀斑都有明显的热层响应。在本研究中，我们进一步探讨了2001-2006年期间所有X级太阳耀斑的热层响应。观测结果表明，X5级和更强的太阳耀斑在耀斑爆发后约4 h内可引起50 ° S-50 ° N热层密度平均增强10-13%。太阳极紫外区的许多重要谱线和连续谱都是光学厚的，因此，由于太阳大气的吸收，位于太阳边缘附近的耀斑的极紫外增强较小。由于太阳极紫外线的临边效应，临边耀斑引起较小的热层响应。热层密度增强与积分EUV通量的相关性比与峰值EUV通量的相关性大得多，相关系数为0.91，这表明热层响应强烈依赖于进入热层的总积分能量。
Previous studies show there are significant thermospheric responses to the two great solar flares on October 28, 2003 (X17.2) and November 4, 2003 (X28). In the present study, we further explored the thermospheric response to all X-class solar flares during 2001-2006. The observed results show that X5 and stronger solar flares can induce an average enhancement of 10-13% in thermospheric density in latitude 50 degrees S-50 degrees N within similar to 4 h after the flare onset. Many important lines and continua in solar EUV region are optically thick, thus EUV enhancements are smaller for flares located near the solar limb due to absorption by the solar atmosphere. Limb flares induce smaller thermospheric responses, due to the limb effect of solar EUV. The thermospheric density enhancement is much more correlated with integrated EUV flux than with peak EUV flux, with a high correlation coefficient of 0.91, which suggests that thermospheric response is strongly dependent on the total integrated energy into the thermosphere.