发表机构
Max-Planck-Institut für Sonnensystemforschung; National Astronomical Observatory of Japan; Instituto de Astrofísica de Andalucía, CSIC（马克斯·普朗克太阳系统研究所; 日本国立天文台; 安达卢西亚天体物理研究所，西班牙高等科学研究委员会）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过MURaM-ChE模拟发现，Sunrise III/SCIP观测到的色球层相反极性侵入普遍存在，源于扭曲磁通绳，揭示色球层磁场结构比预期更复杂。
AI 中文摘要
搭载于气球载Sunrise III天文台的Sunrise色球红外光谱偏振仪（SCIP）在Ca II 854.2 nm谱线提供了太阳色球层的新高分辨率观测。发现磁网络区域中的Stokes-V信号显示出精细结构细节，这表明网络上方的磁场并非简单地作为单极性特征扩展，而是表现出相反极性侵入（OPIs）。这些特征在Stokes-V观测中呈现为细长结构。在本工作中，我们证明此类特征在太阳色球层的数值模拟中普遍出现。我们使用最近开发的MURaM色球扩展版（MURaM-ChE）计算的模拟，其类似于增强网络区域。我们发现OPIs在表面上约1 Mm处的磁场垂直分量中普遍出现，并在Ca II 854.2 nm谱线的合成Stokes-V信号中可见。这些结构的长度为2 Mm至7 Mm，宽度约为1 Mm。与OPI特征相关的磁场构型似乎属于扭曲磁通绳（TFRs），并且在所呈现的21分钟时间序列中大部分时间可见。我们的结果表明，色球层的磁结构比以前认为的更复杂，即使是看似简单的磁通管也显示出嵌入的、指向相反方向的扭曲磁场。这可能有助于解释Sunrise III任务的新高分辨率观测。
英文摘要
The Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) instrument onboard the balloon-borne Sunrise III observatory provided new high-resolution observations of the solar chromosphere in the Ca II 854.2 nm line. The Stokes-V signal in magnetic network regions was found to show fine-structured details, which suggests the magnetic field above the network elements does not simply expand as a unipolar feature but displays opposite-polarity-intrusions (OPIs). These features appear as elongated structures in Stokes-V observations. In this work, we demonstrate that such features appear ubiquitously in a numerical simulation of the solar chromosphere. We use a simulation that is computed with the recently developed chromospheric extension of MURaM (MURaM-ChE) and resembles an enhanced network region. We find that OPIs appear ubiquitously in the vertical component of the magnetic field at around 1 Mm above the surface and are visible in the synthetic Stokes-V signal of the Ca II 854.2 nm line. The structures have lengths of 2 Mm to 7 Mm and widths of approximately 1 Mm. The magnetic field configurations associated with the OPI features appear to belong to twisted flux ropes (TFRs) and are visible for most of the time in the presented 21 min time series. Our results show that the magnetic structure of the chromosphere is more complex than previously thought, with even seemingly simple flux tubes showing embedded twisted fields pointing in the opposite direction. This may help in explaining new high-resolution observations from the Sunrise III mission.
Comments13 pages, 9 figures, published in ApJL as part of the Sunrise III special issue, Arxiv version not language-edited
Journal ref2026 ApJL 1008 L18
