MHD Wave Modes Resolved in Fine‐Scale Chromospheric Magnetic Structures
MHD Wave Modes Resolved in Fine‐Scale Chromospheric Magnetic Structures
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DOI：
10.1002/9781119055006.ch25
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发表时间：
2015-05
期刊：
影响因子：
--
通讯作者：
G. Verth;D. Jess
中科院分区：
文献类型：
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作者：
G. Verth;D. Jess
在过去的十年中，由于显着改善的空间和时间分辨率的色球数据，磁流体动力学（MHD）波在这个迷人的太阳大气层的研究已经上升到太阳物理学研究的前沿。在这篇综述中，我们开始审查的挑战和辩论，表现在有关MHD波模式识别在精细尺度色球磁结构，包括针状，纤维和斑点。接下来，我们继续讨论如何准确识别MHD波模式的过程中也有一个至关重要的作用，估计他们的波能通量。这对于估计MHD波对太阳大气加热的可能贡献至关重要。最后，我们详细介绍了如何在色球MHD波研究的进展也使我们能够，第一次，实施尖端的磁震技术，提供了新的见解低太阳大气层的次分辨率等离子体结构。
Within the last decade, due to significant improvements in the spatial and temporal resolution of chromospheric data, magnetohydrodynamic (MHD) wave studies in this fascinating region of the Sun's atmosphere have risen to the forefront of solar physics research. In this review we begin by reviewing the challenges and debates that have manifested in relation to MHD wave mode identification in fine-scale chromospheric magnetic structures, including spicules, fibrils and mottles. Next we go on to discuss how the process of accurately identifying MHD wave modes also has a crucial role to play in estimating their wave energy flux. This is of cardinal importance for estimating what the possible contribution of MHD waves is to solar atmospheric heating. Finally, we detail how such advances in chromospheric MHD wave studies have also allowed us, for the first time, to implement cutting-edge magnetoseismological techniques that provide new insight into the sub-resolution plasma structuring of the lower solar atmosphere.