太阳活动区暗条的磁场诊断
Magnetic field diagnostics of a solar active region filament
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中文总结 AI 辅助
本研究通过光谱偏振观测和HAZEL反演，诊断了太阳活动区暗条的磁场结构，发现平均场强约101高斯且水平场平行于暗条轴，并揭示了类塞曼轮廓在光学厚区域的局限性，为未来辐射转移建模提供了方向。
中文摘要 AI 辅助
我们对活动区暗条在He I 10830埃和Si I 10827埃谱线中进行了光谱偏振观测，以研究其磁场结构。我们使用HAZEL代码进行了全斯托克斯反演，该代码考虑了塞曼效应和汉勒效应。结果，我们得到了平均磁场强度为101±33高斯，水平磁场几乎平行于暗条轴，使得经典的正常极性和反向极性两种模型之间的区别在物理上变得不显著。此外，我们在观测的某些像素中发现了线性偏振中的类塞曼特征，其特征为双峰对称轮廓。由于这些轮廓无法通过同时包含塞曼和汉勒效应的建模很好地再现，我们假设仅存在塞曼效应进行了反演。反演得到了约500高斯的强磁场。然而，Si I 10827埃的同步观测表明光球磁场弱于100高斯。因此，Diaz Baso等人（2016）提出的场景——即从He I 10830埃推断出的强磁场源于下方光球的污染——不适用于我们的暗条。类塞曼轮廓优先出现在光学厚区域（τ~1.4-2.5），在这些区域，HAZEL中采用的简化假设预计会变得不太可靠。我们的结果表明，这些轮廓揭示了当前反演框架在光学厚区域的局限性，并促使未来进行包含自洽辐射场、多重态组分的差分照明以及可能的频率部分重分布的辐射转移建模。
英文摘要
We performed spectropolarimetric observations of an active region filament in He I 10830 angstrom and Si I 10827 angstrom lines to investigate its magnetic field structure. We carried out full-Stokes inversions with the HAZEL code, which takes into account the Zeeman and Hanle effects. As a result, we yielded a mean field strength of 101 $\pm$ 33 G and a horizontal field nearly parallel to the filament axis, such that the distinction between the two classical normal- and reverse-polarity models becomes physically insignificant. In addition, we found Zeeman-like signatures in the linear polarization, characterized by double-peaked symmetric profiles, in some pixels of our observations. Since these profiles could not be well reproduced by modeling that included both the Zeeman and Hanle effects, we performed inversions assuming only the Zeeman effect. The inversion yielded a strong magnetic field of approximately 500 G. However, simultaneous observations of Si I 10827 angstrom indicate a photospheric magnetic field weaker than 100 G. Therefore, the scenario proposed by Diaz Baso et al. (2016), in which the strong field inferred from He I 10830 angstrom originates from contamination by the underlying photosphere, does not apply to our filament. The Zeeman-like profiles are preferentially found in optically thick regions ($τ$ ~ 1.4-2.5), where the simplifying assumptions adopted in HAZEL are expected to become less reliable. Our results suggest that these profiles reveal limitations of the current inversion framework in optically thick regions and motivate future radiative-transfer modeling incorporating self-consistent radiation fields, differential illumination of the multiplet components, and possibly partial frequency redistribution.
发表机构
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency（宇宙科学研究所）
- Astronomical Observatory, Kyoto University（京都大学天文台）
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