AI 中文总结
研究利用太阳轨道器上的EUI，通过高分辨率观测测量日冕环中传播扰动的特性及起源。核心方法是使用特定序列沿日冕环狭缝测量相关参数。主要贡献是区分出快速和慢速PDs，并分析了它们的不同特性及物理机制。
AI 中文摘要
太阳轨道器任务的近期高分辨率观测有助于探测最小尺度加热的间接特征。本文利用太阳轨道器/EUI在最小可分辨尺度下测量日冕环强度中传播扰动（PDs）的特性并研究其物理起源。使用了高空间（低至每像素125公里）和时间分辨率（5秒 cadence）的两个EUI/HRIEUV序列，沿13个活动区日冕环放置狭缝，测量了PDs在天空平面（PoS）的速度、强度扰动阻尼及周期性。报告了检测到PoS速度在500至2000公里/秒之间的快速PDs，仅在日冕环上部可见，强度增加约为HRIEUV强度的4%至8%，且强度随距离几乎无衰减；还测量到与快速PDs相关的2分钟傅里叶功率谱峰值。快速PDs与较低PoS速度（70至90公里/秒）的慢速PDs在同一日冕环中被检测到，慢速PDs仅在日冕环下部可见且有明显强度阻尼，其特性与慢磁声模式或上升流一致，而快速PDs不能用慢磁声模式解释，其特性与磁重联诱导的快速流、传播横向振荡产生的电流片以及快速磁流体动力学模式或阿尔文波一致。
英文摘要
Recent high-resolution observations from the Solar Orbiter mission can help detect the indirect signatures of heating at the smallest scales. In this work we measure the properties and investigate the physical origin of propagating disturbances (PDs) in the intensity at the smallest resolvable scales with Solar Orbiter/EUI along coronal loops. We used two sequences of EUI/HRIEUV at high spatial (down to 125 km per pixel) and temporal resolutions (5 s of cadence). We placed slits along 13 active region (AR) coronal loops. We measured the plane-of-sky (PoS) velocities and the intensity perturbation damping along the slits of PDs. We also measured the periodicity of PDs in one slit by using a Fourier analysis. We report the detection of PDs that have high PoS velocities ranging between 500 and 2000 km/s (which we call "fast" PDs). They are only visible in the upper part of the coronal loops. The intensity increase associated with these fast PDs is on the order of 4\% to 8\% of the HRIEUV intensity, and we measured little to no damping of their intensity with distance. We also measured a peak in the Fourier power spectra at 2 min above the 95\% confidence limit that is associated with fast PDs. The fast PDs are detected in the same coronal loops as PDs with a lower PoS velocity (70 to 90 kms/s), which we refer to as "slow" PDs. Unlike the fast PDs, these slow PDs are only visible in the lower part of the coronal loop, and they show clear intensity damping. Slow PDs show properties consistent with slow magneto-acoustic modes or upflows. On the other hand, fast PDs cannot be explained by slow magneto-acoustic modes. Instead, they show properties consistent with fast flows induced by magnetic reconnection, current sheet generated by propagating transverse oscillations, and fast magnetohydrodynamics modes or Alfvén waves.
Comments17 pages, 15 figures, 1 table, accepted in A&A on 15/07/2026
DOI：10.1051/0004-6361/202660882
