Coronal mass ejections (CMEs) were discovered in the early 1970s when space-borne coronagraphs revealed that eruptions of plasma are ejected from the Sun. Today, it is known that the Sun produces eruptive flares, filament eruptions, coronal mass ejections and failed eruptions; all thought to be due to a release of energy stored in the coronal magnetic field during its drastic reconfiguration. This review discusses the observations and physical mechanisms behind this eruptive activity, with a view to making an assessment of the current capability of forecasting these events for space weather risk and impact mitigation. Whilst a wealth of observations exist, and detailed models have been developed, there still exists a need to draw these approaches together. In particular more realistic models are encouraged in order to asses the full range of complexity of the solar atmosphere and the criteria for which an eruption is formed. From the observational side, a more detailed understanding of the role of photospheric flows and reconnection is needed in order to identify the evolutionary path that ultimately means a magnetic structure will erupt.

中文翻译：

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太阳爆发的起源、早期演化和可预测性

日冕物质抛射 (CME) 是在 1970 年代初期发现的，当时太空日冕仪显示等离子体喷发是从太阳中喷射出来的。今天，众所周知，太阳会产生喷发耀斑、丝状喷发、日冕物质抛射和失败的喷发；所有这些都被认为是由于日冕磁场在剧烈重构过程中释放了储存在日冕磁场中的能量。本次审查讨论了这种喷发活动背后的观测和物理机制，以评估当前为空间天气风险和影响减轻预测这些事件的能力。尽管存在大量观察结果，并且已经开发了详细的模型，但仍然需要将这些方法结合在一起。特别是鼓励更现实的模型，以评估太阳大气的全方位复杂性以及形成喷发的标准。从观测方面来看，需要更详细地了解光球层流动和重联的作用，以确定最终意味着磁结构将爆发的演化路径。