Weak Damping of Propagating MHD Kink Waves in the Quiescent Corona
Weak Damping of Propagating MHD Kink Waves in the Quiescent Corona
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DOI：
10.3847/1538-4357/ac324d
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发表时间：
2021-05
期刊：
影响因子：
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通讯作者：
R. Morton;A. Tiwari;T. Van Doorsselaere;J. McLaughlin
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文献类型：
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作者：
R. Morton;A. Tiwari;T. Van Doorsselaere;J. McLaughlin
传播的横波被认为是坡印廷通量在整个太阳大气中的关键传输者。最近的研究表明，这些横向运动，解释为磁流体动力学扭结模式，是普遍存在的整个日冕。相关的能量估计表明，这些波携带的能量足以满足静止太阳中日冕辐射损失的需求。然而，目前还不清楚波是如何存款到日冕等离子体的能量。我们提出了一个大规模的研究结果，传播扭结波在静止的日冕使用的数据从日冕多通道偏振仪（CoMP）。分析表明，扭结波似乎是弱阻尼，这意味着低速率的能量转移从大尺度的横向运动到较小的尺度，通过uniturbulence或共振吸收。这就提出了一个问题，即观察到的扭结模式如何将它们的能量存款到日冕等离子体中。此外，这些观察，结合蒙特卡罗模拟的结果，导致我们推断，太阳日冕显示的密度比谱，与较小的密度比（相对于周围的日冕）在静止的日冕环和较高的密度比在活跃区日冕环。
Propagating transverse waves are thought to be a key transporter of Poynting flux throughout the Sun’s atmosphere. Recent studies have shown that these transverse motions, interpreted as the magnetohydrodynamic kink mode, are prevalent throughout the corona. The associated energy estimates suggest the waves carry enough energy to meet the demands of coronal radiative losses in the quiescent Sun. However, it is still unclear how the waves deposit their energy into the coronal plasma. We present the results from a large-scale study of propagating kink waves in the quiescent corona using data from the Coronal Multi-channel Polarimeter (CoMP). The analysis reveals that the kink waves appear to be weakly damped, which would imply low rates of energy transfer from the large-scale transverse motions to smaller scales via either uniturbulence or resonant absorption. This raises questions about how the observed kink modes would deposit their energy into the coronal plasma. Moreover, these observations, combined with the results of Monte Carlo simulations, lead us to infer that the solar corona displays a spectrum of density ratios, with a smaller density ratio (relative to the ambient corona) in quiescent coronal loops and a higher density ratio in active-region coronal loops.