太阳极区日冕中具有大量能量的高频磁流体动力学波
High-Frequency Magnetohydrodynamic Waves with Substantial Energy in the Solar Polar Corona
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中文总结 AI 辅助
研究太阳极区日冕中快速太阳风加速加热问题，利用太阳轨道器极紫外成像仪识别高频MHD波，分析其周期和能量通量，发现高频MHD波可能对太阳极区日冕能量收支有重要贡献，凸显高分辨率观测的价值。
中文摘要 AI 辅助
快速太阳风的加速和加热一直是空间物理学中长期存在的挑战。一种主要理论模型认为高频磁流体动力学（MHD）波在日冕中传输和耗散足够能量。但这种具有显著能量振幅的高频波从未被明确观测到，理论与观测存在关键差距。利用太阳轨道器极紫外成像仪的高频率、高分辨率极紫外成像，在太阳极区日冕羽状物中识别出先前隐藏的高频MHD波群体。对检测到的传播扭结波分析表明，超过三分之一周期短于100秒，此前仪器大多未检测到。功率谱分析显示这些高频波携带大量能量通量，在低频率数据中被严重低估。这些结果表明高频MHD波可能对太阳极区日冕能量收支有重要贡献，可能在太阳风加速中起作用，凸显高分辨率观测对探测磁化空间和天体物理等离子体能量传输的价值。
英文摘要
The acceleration and heating of the fast solar wind remain long-standing challenges in space physics. One type of leading theoretical models requires high-frequency magnetohydrodynamic (MHD) waves to transport and dissipate sufficient energy in the corona. However, such high-frequency waves with energetically significant amplitudes have never been unambiguously observed, leaving a key gap between theories and observations. Using high-cadence, high-resolution extreme-ultraviolet imaging from Solar Orbiter's Extreme Ultraviolet Imager, we identify a previously hidden population of high-frequency MHD waves in coronal plumes of the solar polar region. An analysis of the detected propagating kink waves shows that over one-third have periods shorter than 100 s, a population largely undetected by earlier instruments. Power spectral analysis demonstrates that these high-frequency waves carry substantial energy flux, which are significantly underestimated in lower-cadence data. These results suggest that high-frequency MHD waves may contribute importantly to the energy budget of the solar polar corona and could play a role in solar wind acceleration, highlighting the value of high-resolution observations for probing energy transport in magnetized space and astrophysical plasmas.
