论文标题
将威尔逊凹陷连接到黑子的磁场
Connecting the Wilson depression to the magnetic field of sunspots
论文作者
论文摘要
背景：在黑子中，与安静的太阳相比，连续光学深度统一的几何高度降低了。这种所谓的威尔逊抑郁症是由斑点内强磁场的洛伦兹力引起的。但是，尚未详细了解威尔逊抑郁症如何与磁场的强度和几何形状或黑子的其他特性有关。 目的：我们旨在研究威尔逊抑郁症对黑子磁场性质的依赖性，以及磁场与斑点周围环境的气压相对于威尔逊凹陷的准确贡献。 方法：我们的研究基于24张光谱扫描，对用Hinode进行的12个单独的黑子进行了扫描。我们使用两者都为每个位置得出了威尔逊抑郁症，这是一种基于最小化磁场差异的最近开发的方法，并且早些时候开发了一种方法，该方法在磁场内的气压与磁性内部的磁压力与安静的太阳中的气压之间实施了平衡，从而忽略了弯曲力的影响。然后，我们通过将两种技术的威尔逊抑郁症相互比较，并将它们与黑子的各种参数（例如它们的大小或磁场强度）进行比较，进行了统计分析。 结果：我们发现，对于具有更强磁场的斑点而言，威尔逊抑郁症变得更大，但没有增加的磁压力所期望的那么多。这表明曲率积分为威尔逊抑郁症提供了重要的贡献，尤其是对于磁场较弱的斑点。我们的结果表明，在平均强度的斑点磁场强度不同的斑点之间，磁场中的磁场几何形状有所不同。
Context: In sunspots, the geometric height of continuum optical depth unity is depressed compared to the quiet Sun. This so-called Wilson depression is caused by the Lorentz force of the strong magnetic field inside the spots. However, it is not understood in detail yet, how the Wilson depression is related to the strength and geometry of the magnetic field or to other properties of the sunspot. Aims: We aim to study the dependence of the Wilson depression on the properties of the magnetic field of the sunspots and how exactly the magnetic field contributes to balancing the Wilson depression with respect to the gas pressure of the surroundings of the spots. Methods: Our study is based on 24 spectropolarimetric scans of 12 individual sunspots performed with Hinode. We derived the Wilson depression for each spot using both, a recently developed method that is based on minimizing the divergence of the magnetic field, and an approach developed earlier that enforces an equilibrium between the gas pressure and the magnetic pressure inside the spot and the gas pressure in the quiet Sun, thus neglecting the influence of the curvature force. We then performed a statistical analysis by comparing the Wilson depression resulting from the two techniques with each other and by relating them to various parameters of the sunspots, such as their size or the strength of the magnetic field. Results: We find that the Wilson depression becomes larger for spots with a stronger magnetic field, but not as much as one would expect from the increased magnetic pressure. This suggests that the curvature integral provides an important contribution to the Wilson depression, particularly for spots with a weak magnetic field. Our results indicate that the geometry of the magnetic field in the penumbra is different between spots with different strengths of the average umbral magnetic field.
