Flares and coronal mass ejections should follow a pattern of build-up and release, with the build-up phase understood as the gradual addition of stress to the coronal magnetic field. Recently Hudson (Mon. Not. Roy. Astron. Soc. 491, 4435, 2020) presented observational evidence for this pattern in two isolated active regions from 1997 and 2006, finding a correlation between the waiting time after the event, and the event magnitude. In this article we systematically search for related evidence in the largest 14 active regions of Solar Cycle 24, chosen as those with peak sunspot area exceeding 1000 millionths of the solar hemisphere (MSH). The smallest of these regions, NOAA 12673, produced the exceptional flares SOL2017-09-06 and SOL2017-09-10. None of these regions showed significant correlations of waiting times and flare magnitudes, although two hinted at such an interval-size relationship. Correlations thus appear to be non-existent or intermittent, depending on presently unknown conditions.

中文翻译：

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太阳耀斑的形成和释放

耀斑和日冕物质抛射应该遵循一种积累和释放的模式，积累阶段被理解为日冕磁场逐渐增加压力。最近，哈德逊 (Mon. Not. Roy. Astron. Soc. 491, 4435, 2020) 提供了 1997 年和 2006 年两个孤立活动区域中这种模式的观测证据，发现事件发生后的等待时间与事件强度之间存在相关性. 在本文中，我们系统地搜索了太阳活动周期 24 中最大的 14 个活动区域的相关证据，这些区域被选为太阳黑子峰值面积超过太阳半球 (MSH) 百万分之一的区域。其中最小的区域 NOAA 12673 产生了特殊的耀斑 SOL2017-09-06 和 SOL2017-09-10。这些区域中没有一个显示等待时间和耀斑强度的显着相关性，尽管有两个暗示了这种间隔大小的关系。因此，相关性似乎不存在或断断续续，这取决于目前未知的情况。