Solar irradiance variability during the October 2003 solar storm period
Solar irradiance variability during the October 2003 solar storm period
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DOI：
10.1029/2004gl019571
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发表时间：
2004-05
影响因子：
5.2
通讯作者：
T. Woods;F. Eparvier;J. Fontenla;J. Harder;G. Kopp;W. McClintock;G. Rottman;B. Smiley;M. Snow-M.-S
中科院分区：
文献类型：
--
作者：
T. Woods;F. Eparvier;J. Fontenla;J. Harder;G. Kopp;W. McClintock;G. Rottman;B. Smiley;M. Snow-M.-S
2003年10月18日至2003年11月5日期间的异常太阳风暴包括140多个耀斑，主要来自两个不同的大型太阳黑子群。在此期间有11次大型X级耀斑，包括2003年10月28日的X17耀斑和2003年11月4日的X28耀斑。X28耀斑是GOES自1976年开始测量太阳X射线以来最大的耀斑。这些耀斑期间的太阳（全圆盘）辐照度由NASA太阳辐射和气候实验（SORCE）航天器和NASA热层、电离层、中间层、能量学和动力学（TIMED）航天器上的仪器观测。在此期间，由于黑暗的大太阳黑子，太阳总辐照度（TSI）前所未有地下降了0.34%。此外，在10月28日的X17（4 B光学）耀斑期间，TSI增加了270 ppm，这是TSI耀斑事件的第一次明确测量。这个X17耀斑的紫外（UV）变化范围从10 nm的约50倍缩短到Mg II 280 nm发射的约10%。紫外耀斑变化的一个有趣的结果是，在X17耀斑期间，H I莱曼-α（121.6 nm）发射的宽翼增加了2倍以上，而莱曼-α发射的核心仅增加了20%。另一个有趣的结果是Si III 120.6 nm发射的时间曲线，它显示在脉冲阶段期间急剧增加了1分钟，增加了17倍。
The extraordinary solar storms between 18 October 2003 and 5 November 2003 include over 140 flares, primarily from two different large sunspot groups. There were 11 large X‐class flares during this period, including an X17 flare on 28 October 2003 and an X28 flare on 4 November 2003. The X28 flare is the largest flare since GOES began its solar X‐ray measurements in 1976. The solar (full‐disk) irradiance during these flares was observed by the instruments aboard the NASA Solar Radiation and Climate Experiment (SORCE) spacecraft and the NASA Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) spacecraft. The total solar irradiance (TSI) dropped by unprecedented 0.34% during this period due to the dark, large sunspots. In addition, the TSI increased by 270 ppm during the X17 (4B optical) flare on 28 October, the first definitive measurement of a TSI flare event. The ultraviolet (UV) variations for this X17 flare range from a factor of about 50 shortward of 10 nm to about 10% for the Mg II 280 nm emission. One interesting result for the UV flare variations is that the broad wings of the H I Lyman‐α (121.6 nm) emission increased by more than a factor of 2 during the X17 flare while the core of the Lyman‐α emission only increased by 20%. Another interesting result is the time profile of the Si III 120.6 nm emission, which shows a sharp 1‐minute long increase by a factor of 17 during the impulsive phase.