林冠磁场在谱区的分层。空间正则化弱场近似方法的约束条件
Stratification of canopy magnetic fields in a plage region. Constraints from a spatially-regularized weak-field approximation method
摘要：
磁场在色球加热问题中的作用仍然是不受限制的。大多数来自数值模型的理论预测都依赖于磁场配置、场强和连通性，其细节尚未通过观测研究得到很好的确定。对色球磁场谱区的高分辨率研究很少或根本不存在。我们的目的是研究谱区磁场矢量的分层。利用瑞典1米太阳望远镜CRISP仪器在Mg I $λ$ 5173、Na I $λ$ 5896和Ca II $λ$ 8542谱线上获得的高空间分辨率全斯托克斯观测数据。基于空间正则化的思想，我们发展了一种空间正则化弱场近似（WFA）方法。该方法允许快速计算扩展视场的磁场图。这种新技术的保真度进行了评估，使用快照从一个现实的三维磁流体动力学模拟。本文导出了谱区光球层到色球层的磁场视线分量的深度分层。磁场集中在光球层的粒间通道，并向色球层水平扩展，填满所有空间，形成天篷。我们的研究结果表明，这个树冠层的下边界必须位于大约400-600公里的光球。在低色球层（$z\approx760$ km），平均冠层总磁场强度为658 G.在$z=1160$ km处，我们估计$<B_\parallel>\approx 417$ G。我们提出了一个修改的WFA，提高其适用性的数据更差的信噪比。这些方法为研究多层磁场观测提供了一种快速可靠的方法，而没有其他反演方法所固有的许多困难。
英文摘要：
The role of magnetic fields in the chromospheric heating problem remains greatly unconstrained. Most theoretical predictions from numerical models rely on a magnetic configuration, field strength and connectivity whose details have not been well established with observational studies. High-resolution studies of chromospheric magnetic fields in plage are very scarce or non-existent in general. Our aim is to study the stratification of the magnetic field vector in plage regions. We use high-spatial resolution full-Stokes observations acquired with CRISP instrument at the Swedish 1-m Solar Telescope in the Mg I $λ$5173, Na I $λ$5896 and Ca II $λ$8542 lines. We have developed a spatially-regularized weak-field approximation (WFA) method based on the idea of spatial regularization. This method allows for a fast computation of magnetic field maps for an extended field of view. The fidelity of this new technique has been assessed using a snapshot from a realistic 3D magnetohydrodynamics simulation. We have derived the depth-stratification of the line-of-sight component of the magnetic field from the photosphere to the chromosphere in a plage region. The magnetic fields are concentrated in the intergranular lanes in the photosphere and expand horizontally toward the chromosphere, filling all the space and forming a canopy. Our results suggest that the lower boundary of this canopy must be located around 400-600 km from the photosphere. The mean canopy total magnetic field strength in the lower chromosphere ($z\approx760$ km) is 658 G. At $z=1160$ km we estimate $<B_\parallel>\approx 417$ G. We propose a modification to the WFA that improves its applicability to data with worse signal-to-noise ratio. These methods provide a quick and reliable way of studying multi-layer magnetic field observations without the many difficulties inherent to other inversion methods.
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