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首页> 外文期刊>Journal of Astrophysics and Astronomy >Propagation of coronal mass ejections from the Sun to the Earth
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Propagation of coronal mass ejections from the Sun to the Earth

机译：日冕物质抛射从太阳传播到地球

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Abstract Coronal mass ejections (CMEs), as they can inject a large amounts of mass and magnetic flux into the interplanetary space, are the primary source of space weather phenomena on the Earth. The present review first briefly introduces the solar surface signatures of the origins of CMEs and then focuses on the attempts to understand the kinematic evolution of CMEs from the Sun to the Earth. CMEs have been observed in the solar corona in white-light from a series of space missions over the last five decades. In particular, LASCO/SOHO has provided almost continuous coverage of CMEs for more than two solar cycles until today. However, the observations from LASCO suffered from projection effects and limited field-of-view (within 30 R⊙documentclass12pt{minimal} usepackage{amsmath} usepackage{wasysym} usepackage{amsfonts} usepackage{amssymb} usepackage{amsbsy} usepackage{mathrsfs} usepackage{upgreek} setlength{oddsidemargin}{-69pt} begin{document}$$R_odot $$end{document} from the Sun). In 2006, the launch of the twin STEREO spacecraft has made possible multiple viewpoints imaging observations, which enabled us to assess the projection effects on CMEs. Moreover, heliospheric imagers (HIs) onboard STEREO continuously observed the large and unexplored distance gap between the Sun and the Earth. Finally, the Earth-directed CMEs that earlier have been routinely identified only near the Earth at 1 AU in in situ observations from ACE and WIND, could also be identified at longitudes away from the Sun–Earth line using the in situ instruments onboard STEREO. We describe the key signatures for the identification of CMEs using in situ observations. Our review presents the frequently used methods for estimation of the kinematics of CMEs and their arrival time at 1 AU using primarily SOHO and STEREO observations. We emphasize the need of deriving the three-dimensional (3D) properties of Earth-directed CMEs from the locations away from the Sun–Earth line. The results improving the CME arrival time prediction at Earth and the open issues holding back progress are also discussed. Finally, we summarize the importance of heliospheric imaging and discuss the path forward to achieve improved space weather forecasting.
机译：摘要 日冕物质抛射（CMEs）可以向行星际空间注入大量的质量和磁通量，是地球空间天气现象的主要来源。本文首先简要介绍了CMEs起源的太阳表面特征，然后重点介绍了CMEs从太阳到地球的运动学演化。在过去的五十年里，在一系列太空任务中，在太阳日冕中以白光观察到了CME。特别是，直到今天，LASCO/SOHO几乎连续覆盖了两个以上的太阳周期的CME。然而，LASCO的观测结果受到投影效应和有限的视野的影响（在30 R⊙documentclass[12pt]{minimal} usepackage{amsmath} usepackage{wasysym} usepackage{amsfonts} usepackage{amssymb} usepackage{amsbsy} usepackage{mathrsfs} usepackage{upgreek} setlength{oddsidemargin}{-69pt} begin{document}$$R_odot $$end{document}）。2006年，双STEREO航天器的发射使多视点成像观测成为可能，这使我们能够评估对CME的投射效应。此外，STEREO上的日光层成像仪（HIs）连续观测到太阳和地球之间巨大且未探索的距离差距。最后，早先在ACE和WIND的原位观测中，通常只在地球附近1天文单位的原位观测中识别出的地球定向CME，也可以使用STEREO上的原位仪器在远离日地线的经度处进行识别。我们描述了使用原位观察来识别CME的关键特征。本文介绍了主要使用SOHO和STEREO观测来估计CME运动学及其到达1 AU时间的常用方法。我们强调需要从远离日地线的位置推导出地球定向CME的三维（3D）特性。还讨论了改进CME到达时间预测的结果以及阻碍进展的开放问题。最后，我们总结了日光层成像的重要性，并讨论了实现改进空间天气预报的前进路径。

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