For almost 20 years the physical nature of globally propagating waves in the solar corona (commonly called “EIT waves”) has been controversial and subject to debate. Additional theories have been proposed over the years to explain observations that did not agree with the originally proposed fast-mode wave interpretation. However, the incompatibility of observations made using the Extreme-ultraviolet Imaging Telescope (EIT) onboard the Solar and Heliospheric Observatory with the fast-mode wave interpretation was challenged by differing viewpoints from the twin Solar Terrestrial Relations Observatory spacecraft and data with higher spatial and temporal resolution from the Solar Dynamics Observatory. In this article, we reexamine the theories proposed to explain EIT waves to identify measurable properties and behaviours that can be compared to current and future observations. Most of us conclude that the so-called EIT waves are best described as fast-mode large-amplitude waves or shocks that are initially driven by the impulsive expansion of an erupting coronal mass ejection in the low corona.

中文翻译：

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了解日冕“EIT 波”的物理性质

近 20 年来，日冕中全球传播的波（通常称为“EIT 波”）的物理性质一直存在争议和争论。多年来，已经提出了其他理论来解释与最初提出的快速模式波解释不一致的观察结果。然而，使用太阳和日光层天文台上的极紫外成像望远镜 (EIT) 进行的观测与快速模式波解释的不兼容受到来自双太阳地球关系观测站的不同观点以及具有更高空间和时间的数据的挑战太阳动力学天文台的分辨率。在本文中，我们重新审视了为解释 EIT 波而提出的理论，以识别可与当前和未来观察结果进行比较的可测量属性和行为。我们大多数人得出的结论是，所谓的 EIT 波最好被描述为快速模式的大振幅波或激波，最初是由低日冕中爆发的日冕物质抛射的脉冲膨胀驱动的。