Statistical study of spatio-temporal distribution of precursor solar flares associated with major flares
Statistical study of spatio-temporal distribution of precursor solar flares associated with major flares
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DOI：
10.1093/mnras/stw859
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发表时间：
2016-04
影响因子：
4.8
通讯作者：
N. Gyenge;N. Gyenge;I. Ballai;T. Baranyi
中科院分区：
文献类型：
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作者：
N. Gyenge;N. Gyenge;I. Ballai;T. Baranyi
本研究的目的是研究M级和X级大耀斑前24小时内的前兆耀斑的时空分布以及后续耀斑的演化。有关耀斑（前兆和后续）的信息由拉马迪高能太阳光谱成像仪（RHESSI）提供。耀斑列表，而主要耀斑是由地球静止业务环境卫星（GOES）系统卫星在2002年至2014年期间观测到的。在一天左右的时间内，伴随耀斑的时空分布随主耀斑类型的不同而有明显的演化差异。空间分布的特征是在大耀斑爆发前4个6h时间间隔内，由黑子群直径归一化的主耀斑与其前兆耀斑之间的距离δ的归一化频率分布。X级耀斑的前兆在大耀斑发生前的半天多时间内呈双峰型空间分布，但在大耀斑发生前约6 h，前兆的空间分布变为对数正态分布。M级耀斑的前兆在每个6h子区间内呈对数正态分布。在每种情况下，活动区中最频繁的前体站点距离主要耀斑站点约为太阳黑子群直径的0.1倍。我们的研究表明，能量的积累比能量的释放更有效，因为前体。
The aim of the present investigation is to study the spatio-temporal distribution of precursor flares during the 24 h interval preceding M- and X-class major flares and the evolution of follower flares. Information on associated (precursor and follower) flares is provided by Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). Flare list, while the major flares are observed by the Geostationary Operational Environmental Satellite (GOES) system satellites between 2002 and 2014. There are distinct evolutionary differences between the spatio-temporal distributions of associated flares in about one-day period depending on the type of the main flare. The spatial distribution was characterized by the normalized frequency distribution of the quantity δ (the distance between the major flare and its precursor flare normalized by the sunspot group diameter) in four 6 h time intervals before the major event. The precursors of X-class flares have a double-peaked spatial distribution for more than half a day prior to the major flare, but it changes to a lognormal-like distribution roughly 6 h prior to the event. The precursors of M-class flares show lognormal-like distribution in each 6 h subinterval. The most frequent sites of the precursors in the active region are within a distance of about 0.1 diameter of sunspot group from the site of the major flare in each case. Our investigation shows that the build-up of energy is more effective than the release of energy because of precursors.