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Kink Oscillations of Coronal Loops
Space Science Reviews ( IF 10.3 ) Pub Date : 2021-08-30 , DOI: 10.1007/s11214-021-00847-2
V. M. Nakariakov 1, 2, 3 , D. Y. Kolotkov 1, 4 , S. A. Anfinogentov 5 , P. Antolin 6 , R. Jain 7 , E. G. Kupriyanova 8 , D. Li 9, 10, 11 , N. Magyar 12 , G. Nisticò 13 , D. J. Pascoe 14 , A. K. Srivastava 15 , J. Terradas 16, 17 , S. Vasheghani Farahani 18 , G. Verth 19 , D. Yuan 20 , I. V. Zimovets 21
Affiliation  

Kink oscillations of coronal loops, i.e., standing kink waves, is one of the most studied dynamic phenomena in the solar corona. The oscillations are excited by impulsive energy releases, such as low coronal eruptions. Typical periods of the oscillations are from a few to several minutes, and are found to increase linearly with the increase in the major radius of the oscillating loops. It clearly demonstrates that kink oscillations are natural modes of the loops, and can be described as standing fast magnetoacoustic waves with the wavelength determined by the length of the loop. Kink oscillations are observed in two different regimes. In the rapidly decaying regime, the apparent displacement amplitude reaches several minor radii of the loop. The damping time which is about several oscillation periods decreases with the increase in the oscillation amplitude, suggesting a nonlinear nature of the damping. In the decayless regime, the amplitudes are smaller than a minor radius, and the driver is still debated. The review summarises major findings obtained during the last decade, and covers both observational and theoretical results. Observational results include creation and analysis of comprehensive catalogues of the oscillation events, and detection of kink oscillations with imaging and spectral instruments in the EUV and microwave bands. Theoretical results include various approaches to modelling in terms of the magnetohydrodynamic wave theory. Properties of kink oscillations are found to depend on parameters of the oscillating loop, such as the magnetic twist, stratification, steady flows, temperature variations and so on, which make kink oscillations a natural probe of these parameters by the method of magnetohydrodynamic seismology.



中文翻译:

冠状环的扭结振荡

日冕环的扭结振荡,即驻留扭结波,是日冕中研究最多的动态现象之一。振荡由脉冲能量释放激发,例如低日冕爆发。典型的振荡周期从几分钟到几分钟不等,并且随着振荡回路主半径的增加而线性增加。它清楚地表明扭结振荡是环路的自然模式,可以描述为驻留的快速磁声波,其波长由环路的长度决定。在两种不同的状态下观察到扭结振荡。在快速衰减状态下,表观位移幅度达到环路的几个小半径。大约几个振荡周期的阻尼时间随着振荡幅度的增加而减少,表明阻尼的非线性特性。在无衰减状态下,振幅小于小半径,驱动程序仍然存在争议。该评论总结了过去十年中获得的主要发现,涵盖了观察和理论结果。观测结果包括创建和分析振荡事件的综合目录,以及使用 EUV 和微波波段的成像和光谱仪器检测扭结振荡。理论结果包括根据磁流体动力波理论进行建模的各种方法。发现扭结振荡的特性取决于振荡回路的参数,例如磁扭曲、分层、

更新日期:2021-08-30
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