Abstract

In this paper, 2046 active regions of solar cycle 23 and 1507 active regions of solar cycle 24 observed during the period from May 1996 to December 2018 have been studied. The sunspot groups are distributed according to the recently proposed magneto-morphological classification. Regular active regions (obeing Hale’s polarity law, Joy’s law, and having a leading sunspot that prevails over the main tail sunspot), irregular sunspot groups, and unipolar spots have been identified. It is shown that regular active regions make the major contribution to the development of the cycle, which is consistent with the magnetic cycle models. The contribution of irregular sunspot groups is about two to five times smaller (at the cycle maxima) and comparable with the contribution of regular active regions in the cycle minima, which may indicate the joint action of the global mean field dynamo and the fluctuation dynamo. The increase in the number of irregular active regions in the southern hemisphere at the second maximum of each of the studied cycles can be explained by weakening of the toroidal field (produced by the global dynamo) and an increase in the contribution of the fluctuation dynamo to their competitive interaction. Comparison of the curves describing the time dependence of the sunspot group asymmetry index of regular and irregular active regions showed that, when the activity moves to the southern hemisphere, regular active regions are ahead irregular active regions by ~1.5–2 years. The application of the magneto-morphological classification made it possible to detect the alternating activity of the northern and southern hemispheres in both studied cycles; the order of a response of the hemispheres changed from cycle to cycle; the opposite priority with respect to each other was observed for regular and irregular active regions in the given cycle. Comparison of our results with the results on the cyclic variations of sunspot groups of simple and complex magnetic configuration in different hemispheres obtained earlier by other authors showed the following. An increase of the toroidal field produced by the global dynamo makes it difficult to detect asymmetry manifestations and to reveal the effect of the fluctuation dynamo on the magnetic tubes of the active regions.

中文翻译：

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太阳周期23和24的周期性变化，磁形态和活动区域的复杂性

摘要

本文研究了1996年5月至2018年12月观测到的2046个太阳周期活动区23和1507个太阳周期活动区24。根据最近提出的磁形态分类来分布黑子群。已经确定了规则的活动区域（遵循黑尔的极性定律，乔伊定律，并且具有领先于主要尾部黑子的领先黑子），不规则黑子组和单极点。结果表明，规则的活动区域对循环的发展起了主要作用，这与磁循环模型是一致的。不规则黑子群的贡献要小大约2到5倍（在最大周期处），并且与最小周期中规则活动区域的贡献相当，这可能表明整体平均场发电机和波动发电机的共同作用。在每个研究周期的第二个最大值中，南半球不规则活动区域数量的增加可以通过减弱环形场（由整体发电机产生）和波动发电机对磁场的贡献增加来解释。他们的竞争互动。比较描述规则活动区和不规则活动区黑子群不对称指数的时间依赖性的曲线表明，当活动向南半球移动时，规则活动区比不规则活动区领先约1.5–2年。磁形态分类法的应用使得有可能在两个研究周期中检测北半球和南半球的交替活动。半球的响应顺序随周期而变化；在给定的周期中，对于规则和不规则的活动区域，观察到彼此相反的优先级。将我们的结果与其他作者较早获得的不同半球中简单和复杂磁性构型的太阳黑子群的周期变化结果进行比较后，得出以下结论。由整体发电机产生的环形场的增加使得难以检测不对称表现并难以揭示波动发电机对有源区的磁管的影响。将我们的结果与其他作者较早获得的不同半球中简单和复杂磁性构型的太阳黑子群的周期变化结果进行比较后，得出以下结论。由整体发电机产生的环形场的增加使得难以检测不对称表现并难以揭示波动发电机对有源区的磁管的影响。我们的研究结果与其他作者较早获得的不同半球中简单和复杂磁性构型的太阳黑子群的周期变化结果的比较表明。由整体发电机产生的环形场的增加使得难以检测不对称表现并难以揭示波动发电机对有源区的磁管的影响。