Solar Prominences: Observations
Solar Prominences: Observations
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DOI：
10.12942/lrsp-2014-1
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发表时间：
2014-03
影响因子：
20.9
通讯作者：
S. Parenti
中科院分区：
文献类型：
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作者：
S. Parenti
日冕是太阳大气最常见的特征之一。它们是在日冕中发现的，但它们比日冕物质温度和密度高100倍，这表明它们与周围环境隔绝了热和压力。由于这些性质，当在光学或EUV冷线中观察时，它们在肢体上显示为明亮的特征。在圆盘上，它们看起来比它们的背景更暗，这表明存在等离子体吸收过程(在这种情况下，它们被称为细丝)。日冕等离子体被嵌入在位于磁反转线上方的磁场环境中，被称为丝状通道。本文旨在为读者提供根据观测推断出的表征这些特殊结构、日冕及其环境的主要元素。其目的也是指出和讨论关于日冕的存在、稳定性和消失的公开问题。综述首先对这些特征和用于观测它们的工具进行了概述。第二节介绍了稳定条件下的大尺度性质，包括细丝形态、热力学参数、磁场和周围日冕空穴的性质。第三节致力于从形态和动力学的角度讨论小尺度的观测特性。第四节介绍日冕形成过程中的观测情况，而第五节则回顾导致日冕消失或爆发的不稳定来源。第六节给出了结论和展望。
Solar prominences are one of the most common features of the solar atmosphere. They are found in the corona but they are one hundred times cooler and denser than the coronal material, indicating that they are thermally and pressure isolated from the surrounding environment. Because of these properties they appear at the limb as bright features when observed in the optical or the EUV cool lines. On the disk they appear darker than their background, indicating the presence of a plasma absorption process (in this case they are called filaments). Prominence plasma is embedded in a magnetic environment that lies above magnetic inversion lines, denoted a filament channel.This paper aims at providing the reader with the main elements that characterize these peculiar structures, the prominences and their environment, as deduced from observations. The aim is also to point out and discuss open questions on prominence existence, stability and disappearance.The review starts with a general introduction of these features and the instruments used for their observation. Section 2 presents the large scale properties, including filament morphology, thermodynamical parameters, magnetic fields, and the properties of the surrounding coronal cavity, all in stable conditions. Section 3 is dedicated to small-scale observational properties, from both the morphological and dynamical points of view. Section 4 introduces observational aspects during prominence formation, while Section 5 reviews the sources of instability leading to prominence disappearance or eruption. Conclusions and perspectives are given in Section 6.