Relationship between Solar Energetic Particles and Properties of Flares and CMEs: Statistical Analysis of Solar Cycle 23 Events
Relationship between Solar Energetic Particles and Properties of Flares and CMEs: Statistical Analysis of Solar Cycle 23 Events
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DOI：
10.1007/s11207-014-0641-4
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发表时间：
2015-03-01
期刊：
影响因子：
2.8
通讯作者：
Tsiropoula, G.
中科院分区：
文献类型：
--
作者：
Dierckxsens, M.;Tziotziou, K.;Tsiropoula, G.
对太阳高能粒子（SEP）与太阳耀斑和日冕物质抛射（CME）的关系进行了统计分析。在太阳活动周期23期间的SEP事件被选择为与起源于太阳的可见半球的太阳耀斑相关联，并且至少为M1级。考虑到所有耀斑和日冕物质抛射发生在这一时期，发生的概率SEP事件在地球附近的确定。一个强大的上升，这一概率观察到耀斑强度增加，更西部的位置，更高的日冕物质抛射速度，和晕日冕物质抛射。质子峰值通量和这些太阳参数之间的相关性推导出了一个低（> 10 MeV）和高（> 60 MeV）的能量范围内，不包括任何通量增强，由于快速行星际冲击的通道。当E > 10 MeV（E > 60 MeV）时，与耀斑强度的相关系数为0.55 +/- 0.07（0.63 +/- 0.06），与CME速度的相关系数为0.56 +/- 0.08（0.40 +/- 0.09）。对于这两个能量范围，与耀斑经度和CME宽度的相关性非常弱或不存在。此外，发生概率，相关系数，和平均峰值通量导出在多维箱结合上述太阳参数。在不同的质子能量通道，从5到200 MeV的相关系数也被确定。结果表明，质子峰值通量与日冕物质抛射速度的相关性随能量的增加而减小，而与耀斑强度的相关性则相反。此外，与CME速度的相关性强于与耀斑强度的相关性，低于15 MeV，并在20 MeV以上变得较弱。当不排除行星际激波引起的通量剖面的增强时，在7 MeV以下的质子峰值通量与CME速度之间的相关系数中只观察到一个很小但不是很显著的变化。
A statistical analysis of the relationship between solar energetic particles (SEPs) and properties of solar flares and coronal mass ejections (CMEs) is presented. SEP events during Solar Cycle 23 are selected that are associated with solar flares originating in the visible hemisphere of the Sun and that are at least of magnitude M1. Taking into account all flares and CMEs that occurred during this period, the probability for the occurrence of an SEP event near Earth is determined. A strong rise of this probability is observed for increasing flare intensities, more western locations, higher CME speeds, and halo CMEs. The correlations between the proton peak flux and these solar parameters are derived for a low (> 10 MeV) and high (> 60 MeV) energy range excluding any flux enhancement due to the passage of fast interplanetary shocks. The obtained correlation coefficients are 0.55 +/- 0.07 (0.63 +/- 0.06) with flare intensity, and 0.56 +/- 0.08 (0.40 +/- 0.09) with CME speed for E > 10 MeV (E > 60 MeV). For both energy ranges, the correlations with flare longitude and CME width are very weak or non-existent. Furthermore, the occurrence probabilities, correlation coefficients, and mean peak fluxes are derived in multi-dimensional bins combining the aforementioned solar parameters. The correlation coefficients are also determined in different proton energy channels ranging from 5 to 200 MeV. The results show that the correlation between the proton peak flux and the CME speed decreases with energy, while the correlation with the flare intensity shows the opposite behaviour. Furthermore, the correlation with the CME speed is stronger than the correlation with the flare intensity below 15 MeV and becomes weaker above 20 MeV. When the enhancements in the flux profiles due to interplanetary shocks are not excluded, only a small but not very significant change is observed in the correlation coefficients between the proton peak flux below 7 MeV and the CME speed.