Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging.

中文翻译：

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大规模全球传播的日冕波。

自1960年代以来，已经在太阳色球层中观测到了大规模的，全球传播的波状扰动，并通过电晕进行了推断。但是，仅从1990年代末以来才对这些现象进行了详细的分析。这是由众多基于间隔的仪器提供的高节奏日冕成像数据推动的，这些数据通常显示出壮观的全球传播的明亮前线。如今，人们通常在广泛的光谱通道中观察到冠冕波，这些冠冕波通常被称为“扰动”，从而产生了大量的信息。许多发现支持对干扰的“经典”解释：在太阳日冕中传播的快速模式MHD波或冲击。然而，看起来与这张图片不一致的观测结果刺激了替代模型的发展，在替代模型中，在扩大的日冕物质抛射的框架内，通过磁重构产生了“伪波”。这引起了关于这些干扰的物理性质的激烈辩论。这篇综述的重点是演示如何使用过去十五年的大量观察结果来约束我们的大型日冕波模型，以及如何最终形成对这些干扰的连贯的物理理解。