Due to the increase in the spatial and temporal resolution of observations of the solar atmosphere, which is mainly associated with progress in space research, we now understand that the Sun’s activity not only is associated with large centers, but also extends to significantly smaller scales. Each new advance in experimental technology over the past 60 years has led to the discovery of more and more numerous and small solar structures: X-ray active regions in the 1960s, hot X-ray points in the 1970s, solar microflares in the 1980s, and finally, from the end of the 20th century, solar nanoflares. At the same time, the total energy release, obtainable from observations, is still insufficient to ensure a balance between heating of the corona and its rapid radiative cooling. For the smallest-scale phenomena, nanoflares, it is still not possible to resolve their structure and mechanism, which raises the question of whether it is correct to classify them as flares. We present a review of the main results obtained so far in the field of small-scale solar activity, mainly microflares and nanoflares, and discuss the main issues that need to be solved in order to move forward.

由于太阳大气观测的空间和时间分辨率的提高，这主要与空间研究的进展有关，我们现在了解到太阳的活动不仅与大中心有关，而且还扩展到明显更小的尺度。过去 60 年来，实验技术的每一项新进步都导致发现越来越多的小型太阳结构：1960 年代的 X 射线活跃区域、1970 年代的热 X 射线点、1980 年代的太阳微耀斑、最后，从 20 世纪末开始，出现了太阳能纳米耀斑。同时，从观测中获得的总能量释放仍不足以确保日冕加热和快速辐射冷却之间的平衡。对于最小尺度的现象，纳米耀斑，仍然无法解决它们的结构和机制，这就提出了将它们归类为耀斑是否正确的问题。我们回顾了迄今为止在小尺度太阳活动领域取得的主要成果，主要是微耀斑和纳米耀斑，并讨论了向前推进需要解决的主要问题.