论文标题
基于日出/IMAX矢量磁图的AR11768的磁液静态建模
Magnetohydrostatic modeling of AR11768 based on a SUNRISE/IMaX vector magnetogram
论文作者
论文摘要
语境。高分辨率磁场测量仅在太阳光球中进行。较高的层，例如色球和电晕，可以通过向上推动光球磁场来建模。在太阳能电晕中，可以忽略等离子力，而洛伦兹的力消失了。在磁性和非磁力同样重要的情况下，在上光球和染色器上并非如此。解决此问题的一种方法是使用磁液静态（MHS）模型自兼容的等离子体和磁场。 目标。我们旨在通过将新开发的外推技术应用于日出/IMAX数据来得出AR11768的磁场，血浆压力和密度。 方法。 MHS建模使用优化方法。初始条件由非线性力场（NLFFF）和重力分层的气氛组成。 结果。在通过新代码在空间上解决的非强度层中，洛伦兹力有效地通过气压梯度力和重力力来平衡。压力和密度在强场区域耗尽，这与观察结果一致。然而，在活性区域边缘的某些部分也观察到了更密集的血浆。在染色体上，原纤维样等离子体结构很好地跟踪磁场。日出/SUFI 3000 {$Å$}图像中的明亮点通常伴随等离子压力和电流浓度。此外，MHS场线与选定的色球纤维之间的平均角度为$ 11.8^\ Circ $，它比从NLFFF型号（$ 15.7^\ circ $）和线性MHS型号（$ 20.9^\ Circ $）计算出的平均值。这表明MHS溶液提供了染色体中磁场的更好表示。
Context. High resolution magnetic field measurements are routinely done only in the solar photosphere. Higher layers like the chromosphere and corona can be modeled by extrapolating the photospheric magnetic field upward. In the solar corona, plasma forces can be neglected and the Lorentz force vanishes. This is not the case in the upper photosphere and chromosphere where magnetic and non-magnetic forces are equally important. One way to deal with this problem is to compute the plasma and magnetic field self-consistently with a magnetohydrostatic (MHS) model. Aims. We aim to derive the magnetic field, plasma pressure and density of AR11768 by applying the newly developed extrapolation technique to the SUNRISE/IMaX data. Methods. An optimization method is used for the MHS modeling. The initial conditions consist of a nonlinear force-free field (NLFFF) and a gravity-stratified atmosphere. Results. In the non-force-free layer, which is spatially resolved by the new code, Lorentz forces are effectively balanced by the gas pressure gradient force and the gravity force. The pressure and density are depleted in strong field regions, which is consistent with observations. Denser plasma, however, is also observed at some parts of the active region edges. In the chromosphere, the fibril-like plasma structures trace the magnetic field nicely. Bright points in SUNRISE/SuFI 3000 {$Å$} images are often accompanied by the plasma pressure and electric current concentrations. In addition, the average of angle between MHS field lines and the selected chromospheric fibrils is $11.8^\circ$, which is smaller than those computed from the NLFFF model ($15.7^\circ$) and linear MHS model ($20.9^\circ$). This indicates that the MHS solution provides a better representation of the magnetic field in the chromosphere.
