Strong solar flares and coronal mass ejections, here defined not only as the bursts of electromagnetic radiation but as the entire process in which magnetic energy is released through magnetic reconnection and plasma instability, emanate from active regions (ARs) in which high magnetic non-potentiality resides in a wide variety of forms. This review focuses on the formation and evolution of flare-productive ARs from both observational and theoretical points of view. Starting from a general introduction of the genesis of ARs and solar flares, we give an overview of the key observational features during the long-term evolution in the pre-flare state, the rapid changes in the magnetic field associated with the flare occurrence, and the physical mechanisms behind these phenomena. Our picture of flare-productive ARs is summarized as follows: subject to the turbulent convection, the rising magnetic flux in the interior deforms into a complex structure and gains high non-potentiality; as the flux appears on the surface, an AR with large free magnetic energy and helicity is built, which is represented by \(\delta \)-sunspots, sheared polarity inversion lines, magnetic flux ropes, etc; the flare occurs when sufficient magnetic energy has accumulated, and the drastic coronal evolution affects magnetic fields even in the photosphere. We show that the improvement of observational instruments and modeling capabilities has significantly advanced our understanding in the last decades. Finally, we discuss the outstanding issues and future perspective and further broaden our scope to the possible applications of our knowledge to space-weather forecasting, extreme events in history, and corresponding stellar activities.

中文翻译：

---

产生耀斑的活跃区域。

强烈的太阳耀斑和日冕物质抛射，在这里不仅定义为电磁辐射的爆发，而且定义为通过磁重联和等离子体不稳定性释放磁能的整个过程，来自高磁非势的活动区域 (AR)存在多种形式。这篇综述从观测和理论的角度着重于耀斑产生 AR 的形成和演变。从总体介绍 AR 和太阳耀斑的成因开始，我们概述了在耀斑前状态的长期演化过程中的关键观测特征，与耀斑发生相关的磁场的快速变化，以及这些现象背后的物理机制。我们对产生耀斑的 AR 的图片总结如下：在湍流对流的作用下，内部上升的磁通量变形为复杂结构，获得高非势；随着磁通量出现在表面，建立了一个自由磁能大、螺旋度大的AR，表示为\(\delta \) -太阳黑子、剪切极性反转线、磁通绳等；当积累了足够的磁能时会发生耀斑，剧烈的日冕演化会影响甚至在光球层中的磁场。我们表明，观测仪器和建模能力的改进在过去几十年中显着提高了我们的理解。最后，我们讨论了悬而未决的问题和未来前景，并进一步扩大了我们的知识范围，将我们的知识应用于空间天气预报、历史上的极端事件和相应的恒星活动。