AI 中文总结
研究利用Sunrise III/SCIP观测宁静太阳网络元，发现其边界含膨胀磁冠结构与寄生极性，为太阳网络元三维磁结构提供新约束。
AI 中文摘要
我们展示了利用Sunrise III色球层红外光谱偏振仪获得的宁静太阳网络元的高分辨率多线光谱偏振观测结果。这些观测结合了光球层、光球上层和色球层的诊断信息，其空间分辨率和偏振灵敏度可直接用于研究网络边界的横向磁结构。我们发现，最强的线偏振集中在磁元边缘的狭窄脊状区域，与通过多线反演推断出的增强横向磁场共空间。磁方位角围绕一个更垂直的核心呈现出连贯、主要为径向的组织，与膨胀的磁冠结构一致。直接从观测到的Fe I和K I线偏振导出的方位角 proxy 再现了相同的大尺度组织，表明该结构编码在斯托克斯轮廓中，而非由反演强加。响应函数和基于MURaM的前向合成测试表明，Fe I 8468 Å线偏振对光球上层的磁方位角敏感，在logτ≈-3附近达到最接近的 proxy 一致性。我们未发现Fe和K敏感诊断之间存在强方位角剪切的证据。在网络边界处，我们还识别出与复杂多瓣斯托克斯V轮廓相关的局域寄生极性斑块，以及一个在光球Fe I线和色球Ca II线之间斯托克斯V极性反转的案例。这些结果表明，宁静太阳网络边界包含有组织的光球上层冠场以及小规模混合极性结构，为网络元的三维磁结构提供了新的约束。
英文摘要
We present high-resolution multi-line spectropolarimetric observations of a quiet-Sun network element obtained with the {\sc Sunrise~iii} Chromospheric Infrared SpectroPolarimeter. The observations combine photospheric, upper-photospheric, and chromospheric diagnostics at a spatial resolution and polarimetric sensitivity that allow the transverse magnetic structure of the network boundary to be examined directly. We find that the strongest linear polarisation is concentrated in a narrow ridge around the edge of the magnetic element, co-spatial with enhanced transverse magnetic field inferred from multiline inversions. The magnetic azimuth exhibits a coherent, predominantly radial organisation around a more vertical core, consistent with an expanding magnetic canopy. An azimuth proxy derived directly from the observed Fe~\textsc{i} and K~\textsc{i} linear polarisation reproduces the same large-scale organisation, showing that this structure is encoded in the Stokes profiles rather than imposed by the inversion. Response functions and a MURaM-based forward-synthesis test indicate that the Fe~\textsc{i}~8468~Å linear polarisation is sensitive to magnetic azimuth in the upper photosphere, with the closest proxy agreement occurring near $\logτ\approx-3$. We find no evidence for strong azimuthal shear between the Fe- and K-sensitive diagnostics. At the network boundary, we also identify localised parasitic-polarity patches associated with complex, multi-lobed Stokes $V$ profiles, and one case in which the Stokes $V$ polarity reverses between photospheric Fe~\textsc{i} and chromospheric Ca~\textsc{ii} lines. These results demonstrate that quiet-Sun network boundaries contain organised upper-photospheric canopy fields together with small-scale mixed-polarity structure, providing new constraints on the three-dimensional magnetic structure of network elements.
CommentsAccepted for publication in ApJL
