Solar eruptive phenomena embrace a variety of eruptions, including flares, solar energetic particles, and radio bursts. Since the vast majority of these are associated with the eruption, development, and evolution of coronal mass ejections (CMEs), we focus on CME observations in this review. CMEs are a key aspect of coronal and interplanetary dynamics. They inject large quantities of mass and magnetic flux into the heliosphere, causing major transient disturbances. CMEs can drive interplanetary shocks, a key source of solar energetic particles and are known to be the major contributor to severe space weather at the Earth. Studies over the past decade using the data sets from (among others) the SOHO, TRACE, Wind, ACE, STEREO, and SDO spacecraft, along with ground-based instruments, have improved our knowledge of the origins and development of CMEs at the Sun and how they contribute to space weather at Earth. SOHO, launched in 1995, has provided us with almost continuous coverage of the solar corona over more than a complete solar cycle, and the heliospheric imagers SMEI (2003–2011) and the HIs (operating since early 2007) have provided us with the capability to image and track CMEs continually across the inner heliosphere. We review some key coronal properties of CMEs, their source regions and their propagation through the solar wind. The LASCO coronagraphs routinely observe CMEs launched along the Sun-Earth line as halo-like brightenings. STEREO also permits observing Earth-directed CMEs from three different viewpoints of increasing azimuthal separation, thereby enabling the estimation of their three-dimensional properties. These are important not only for space weather prediction purposes, but also for understanding the development and internal structure of CMEs since we view their source regions on the solar disk and can measure their in-situ characteristics along their axes. Included in our discussion of the recent developments in CME-related phenomena are the latest developments from the STEREO and LASCO coronagraphs and the SMEI and HI heliospheric imagers.

中文翻译：

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冠状物质抛射：观察

太阳爆发现象包括各种爆发，包括耀斑，太阳高能粒子和无线电爆发。由于其中绝大多数与冠状物质抛射（CME）的爆发，发展和演化有关，因此在本综述中我们将重点介绍CME的观测结果。CME是日冕和行星际动力学的关键方面。它们将大量的质量和磁通量注入日光层，从而引起重大的瞬态干扰。CME可以驱动行星际冲击，这是太阳高能粒子的关键来源，并且众所周知，CME是造成地球严酷太空天气的主要因素。在过去十年中使用SOHO，TRACE，Wind，ACE，STEREO和SDO航天器以及其他地面仪器的数据集进行了研究，提高了我们对CME在太阳上的起源和发展以及它们如何对地球太空天气的影响的了解。自1995年启动以来，SOHO不仅为我们提供了超过一个完整太阳周期的几乎连续的太阳日冕覆盖范围，而且日光层成像仪SMEI（2003-2011年）和HIs（自2007年初开始运行）为我们提供了能力连续成像并跟踪整个日球内部的CME。我们回顾了CME的一些关键冠冕特性，它们的源区以及它们在太阳风中的传播。LASCO日冕仪通常会观察到沿日地线发射的CME，像光晕一样变亮。STEREO还允许从增加方位角间隔的三种不同角度观察地球定向CME，从而能够估算其三维特性。这些不仅对于空间天气预报目的很重要，而且对于理解CME的发展和内部结构也很重要，因为我们在太阳圆盘上观察了它们的源区并可以测量其沿轴的原位特征。在我们对CME相关现象的最新发展的讨论中，包括STEREO和LASCO日冕仪以及SMEI和HI日球成像仪的最新发展。