Intensity variation of large solar energetic particle events associated with coronal mass ejections
Intensity variation of large solar energetic particle events associated with coronal mass ejections
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DOI：
10.1029/2004ja010602
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发表时间：
2004-12
影响因子：
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通讯作者：
N. Gopalswamy;S. Yashiro;S. Krucker;G. Stenborg;R. Howard
中科院分区：
文献类型：
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作者：
N. Gopalswamy;S. Yashiro;S. Krucker;G. Stenborg;R. Howard
[1]我们研究了1996-2002年第23太阳活动周（1996-2002）与太阳高能粒子（SEP）事件相关的日冕物质抛射（CME）和耀斑，以确定太阳爆发的什么性质可能决定SEP强度。SEP事件被分为三组：（1）在主CME之前有一个或多个来自同一太阳源的宽CME的事件，（2）没有这样的CME之前的事件，和（3）主CME可能与流光或附近的晕CME相互作用的事件。尽管CME性质几乎相同，但第1组和第2组的SEP强度不同。第3组与第1组相似。主要结果如下：（1）同一源区的CME前有一次大范围的CME时，SEP的强度较高。(2)高强度SEP事件的平均耀斑大小也较大。(3)SEP事件的强度与先前的CME表现出更紧密的相关性与CME的速度。当单独考虑不同亚组时，CME速度与SEP强度图的分散程度降低。(4)高能电子的强度与耀斑的大小比与CME速度有更好的相关性。(5)SEP强度与耀斑大小的相关性较差，第3组事件除外。由于只有三分之一的事件没有之前的CME，我们的结论是，大多数的SEP产生CME传播通过近太阳行星际介质严重干扰和扭曲的前CME。此外，之前的CME平均速度更快，范围更广，因此它们可能为随后的CME驱动的冲击提供种子粒子。因此，我们得出结论，不同强度的SEP事件在这两个群体中可能没有导致由于CME的固有属性。先前CME的存在似乎是区分高强度和低强度SEP事件的特征。
[1] We studied the coronal mass ejections (CMEs) and flares associated with large solar energetic particle (SEP) events of solar cycle 23 (1996–2002) in order to determine what property of the solar eruptions might order the SEP intensity. The SEP events were divided into three groups: (1) events in which the primary CME was preceded by one or more wide CMEs from the same solar source, (2) events with no such preceding CMEs, and (3) events in which the primary CME might have interacted with a streamer or with a nearby halo CME. The SEP intensities are distinct for groups 1 and 2 although the CME properties were nearly identical. Group 3 was similar to group 1. The primary findings of this study are as follows: (1) Higher SEP intensity results whenever a CME is preceded by another wide CME from the same source region. (2) The average flare size was also larger for high-intensity SEP events. (3) The intensity of SEP events with preceding CMEs showed a tighter correlation with CME speed. The extent of scatter in the CME speed versus SEP intensity plots was reduced when various subgroups were considered separately. (4) The intensities of energetic electrons were better correlated with flare size than with CME speed. (5) The SEP intensity showed poor correlation with the flare size, except for group 3 events. Since only a third of the events did not have preceding CMEs, we conclude that the majority of SEP producing CMEs propagate through the near-Sun interplanetary medium severely disturbed and distorted by the preceding CMEs. Furthermore, the preceding CMEs are faster and wider on the average, so they may provide seed particles for CME-driven shocks that follow. Therefore we conclude that the differing intensities of SEP events in the two groups may not have resulted due to the inherent properties of the CMEs. The presence of preceding CMEs seems to be the discriminating characteristic of the high- and low-intensity SEP events.