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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Flare location on the solar disk: Modeling the thermosphere and ionosphere response
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Flare location on the solar disk: Modeling the thermosphere and ionosphere response

机译：太阳能磁盘上光斑位置:建模热电离层和电离层响应

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Solar flare enhancements to the soft X-ray (XUV) and extreme ultraviolet (EUV) spectral irradiance depend on the location of the flare on the solar disk. Most emission lines in the XUV region (～0.1 to ～25 nm) are optically thin and are weakly dependent on the location of the flare, but in the EUV region (～25 to ～120 nm), many important lines and continua are optically thick, so enhancements are relatively smaller for flares located near the solar limb, due to absorption by the solar atmosphere. The flare irradiance spectral model (FISM) was used to illustrate these location effects, assuming two X17 flares that are identical except that one occurs near disk center and the other near the limb. FISM spectra of these two flares were used as solar input to the National Center for Atmospheric Research (NCAR) thermosphere-ionosphere-mesosphere electrodynamics general circulation model (TIME-GCM) to investigate the ionosphere/thermosphere (I/T) response. Model simulations showed that in the E region ionosphere, where XUV dominates ionization, flare location does not affect I/T response. However, flare-driven changes in the F region ionosphere, total electron content (TEC), and neutral density in the upper thermosphere, are 2-3 times stronger for a disk-center flare than for a limb flare, due to the importance of EUV enhancement. Flare location did not affect the timing of the ionospheric response, but the thermospheric response was ～20 mm faster for the disk-center flare. Model simulations of UT responses to an X17 flare on 28 October 2003 were consistent with measurements of TEC and neutral density changes.
机译：太阳耀斑对软x射线的增强(远紫外线)和极端紫外光谱辐照度(EUV)取决于在太阳耀斑的位置磁盘。~ 25海里)光学薄而弱依赖于耀斑的位置,但在EUV地区(~ 25 ~ 120海里),许多重要的线和连续光学厚,所以增强对耀斑相对较小位于太阳能翼附近,由于吸收了太阳的大气层。光谱模型(FISM)被用来说明这些位置效应,假设两个X17耀斑是相同的,除了一个附近发生磁盘中心和附近的其他肢体。这两个耀斑被用作太阳能光谱国家中心的大气的输入研究(NCAR)thermosphere-ionosphere-mesosphere电动力学环流模式(TIME-GCM)调查电离层/热电离层(I / T)的反应。模拟显示,在E地区电离层,远紫外线主宰电离,耀斑位置不影响I / T响应。flare-driven F地区电离层的变化,总电子含量(TEC)和中性密度上热电离层,2 - 3倍对于一个圆心比肢体耀斑爆发,由于EUV增强的重要性。位置没有影响的时机电离层响应,但thermospheric反应是~ 20毫米为圆心更快耀斑。X17闪耀2003年10月28日是一致的测量TEC和中性密度变化。

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