发表机构
Queen’s University Belfast; Max Planck Institute for Solar System Research; California State University Northridge; ASI Italian Space Agency; University of Glasgow; University of Oslo; Universidade Presbiteriana Mackenzie（贝尔法斯特女王大学; 马克斯·普朗克太阳系统研究所; 北岭加州州立大学; 意大利航天局; 格拉斯哥大学; 奥斯陆大学; 麦肯齐长老会大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用 Sunrise III/SUSI 观测发现，C8.2 耀斑后约 30 分钟，磁孔中 4.2-7.0 mHz 振荡功率增强 1.60-8.71 倍，而 7.0-11.5 mHz 功率降低，揭示耀斑引起的波传播变化。
AI 中文摘要
渗透太阳大气的磁振荡可能因耀斑而改变，其原因可能是大气磁波导、热力学分层或两者同时发生变化。为探究此问题，我们利用 Sunrise III 搭载的 Sunrise 紫外光谱偏振成像仪（SUSI）的观测数据，研究了被 C8.2 耀斑条带部分穿越的磁孔中的振荡。我们追踪了 327-329 nm 波段内八条谱线的核心强度，并显示在耀斑峰值后约 30 分钟测量的 4.2-7.0 mHz 范围内的振荡功率，在全部八条谱线中均超过事件前值，增幅因子为 1.60-8.71。相反，在 7.0-11.5 mHz 频段，事件后的强度功率较低——在七条观测谱线中约为原始功率的 0.13-0.41。谱线中心速度测量支持低频增强。这种向低频段的延迟、谱线依赖的转移与耀斑引起的波传播、反射或共振响应变化一致，尽管热力学和磁效应目前尚无法区分。
英文摘要
Magnetic oscillations permeating the solar atmosphere can be altered by flares. This could be due to changes in the atmospheric magnetic waveguide, the thermodynamic stratification, or both. To investigate this, we examine oscillations in a magnetic pore crossed in part by the ribbon of a C8.2 flare, using observations from the Sunrise Ultraviolet Spectropolarimeter and Imager (SUSI) aboard Sunrise III. We track the core intensities of eight spectral lines between 327-329 nm and show that oscillatory power in the 4.2-7.0 mHz range, measured around 30 minutes after the flare peak, exceeds the pre-event value in all eight lines by factors of 1.60-8.71. Conversely, in the 7.0-11.5 mHz band, the post-event intensity power is lower - approximately 0.13-0.41 of the original power in seven of the observed lines. Line-center velocity measurements support the lower-frequency enhancement. This delayed, line-dependent shift toward the lower-frequency band is consistent with flare-induced changes in wave transmission, reflection, or resonant response, although thermodynamic and magnetic effects cannot yet be separated.
CommentsAccepted for publication in The Astrophysical Journal Letters
