Inference of magnetic fields in the very quiet Sun
Inference of magnetic fields in the very quiet Sun
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非常安静的太阳中的磁场推断
DOI：
10.1051/0004-6361/201628449
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
R. Volkmer
中科院分区：
文献类型：
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作者：
M. Gonz'alez;A. P. Yabar;A. Lagg;A. Ramos;M. Collados;S. Solanki;H. Balthasar;T. Berkefeld;C. Denker;H. Doerr;A. Feller;M. Franz;S. J. G. Manrique;A. Hofmann;F. Kneer;C. Kuckein;R. Louis;O. V. D. Luuhe;H. Nicklas;D. Orozco;R. Rezaei;R. Schlichenmaier;D. Schmidt;W. Schmidt;M. Sigwarth;M. Sobotka;D. Soltau;J. Staude;K. Strassmeier;M. Verma;T. Waldman;R. Volkmer
我们提出了高精度的光谱偏振数据与高空间分辨率（0.4 $“$）的非常安静的太阳在1.56 $\mu $m的格里戈尔望远镜，以阐明这个复杂的磁性。我们所观察到的宁静太阳区域的一半是更好地解释了磁子结构内的分辨率元素。然而，我们无法区分这种子结构是来自于物理参数沿着视线的梯度还是来自于水平梯度（穿过表面）。在这些像素中，具有两个磁分量的模型是优选的，并且我们发现两个不同的磁场种群。填充因子较大的人口有非常弱（150 G）的水平领域类似于以前的作品中获得的。我们证明，这个人口的场矢量是不受约束的意见，我们的数据的空间分辨率和极化精度。具有较小填充因子的其他组件的拓扑结构受到250 G以上场强的观测的约束：我们推断具有与各向同性分布兼容的倾角和方位角值的hG场。填充因子通常低于30%。我们还发现，两极的流量是不平衡的。从另一半的观测安静的太阳区域$50\%是两个lobed斯托克斯$V$配置文件，这意味着23\%的视野可以充分解释与一个单一的恒定磁场嵌入在非磁性的气氛。根据规则剖面，磁场矢量和填充因子的可信度仅为50%。因此，12%的视场具有填充因子通常低于30%的hG场。在我们目前的空间分辨率下，70%的像素显然是非磁化的。
We present high-precision spectro-polarimetric data with high spatial resolution (0.4$''$) of the very quiet Sun at 1.56$\mu$m obtained with the GREGOR telescope to shed some light on this complex magnetism. Half of our observed quiet-Sun region is better explained by magnetic substructure within the resolution element. However, we cannot distinguish whether this substructure comes from gradients of the physical parameters along the line of sight or from horizontal gradients (across the surface). In these pixels, a model with two magnetic components is preferred, and we find two distinct magnetic field populations. The population with the larger filling factor has very weak ($\sim$150 G) horizontal fields similar to those obtained in previous works. We demonstrate that the field vector of this population is not constrained by the observations, given the spatial resolution and polarimetric accuracy of our data. The topology of the other component with the smaller filling factor is constrained by the observations for field strengths above 250 G: we infer hG fields with inclinations and azimuth values compatible with an isotropic distribution. The filling factors are typically below 30\%. We also find that the flux of the two polarities is not balanced. From the other half of the observed quiet-Sun area $\sim$50\% are two-lobed Stokes $V$ profiles, meaning that 23\% of the field of view can be adequately explained with a single constant magnetic field embedded in a non-magnetic atmosphere. The magnetic field vector and filling factor are reliable inferred in only 50\% based on the regular profiles. Therefore, 12\% of the field of view harbour hG fields with filling factors typically below 30\%. At our present spatial resolution, 70\% of the pixels apparently are non-magnetised.