Abstract

The paper presents a modified version of a previously published 3D model of the solar facular knot (Solov’ev and Kirichek, 2019), which successfully describes the main structural features of the solar facular formations. As in the main model, we use the solution (Schatzman, 1965) in the potential approximation as the basis of the magnetic structure of the facular element. The magnetic profile of the facula, as before, has the shape of a fountain, in which thin streams of plasma rise in the center of the node and flow on its periphery along magnetic field lines. This configuration is very similar to the observed patterns (Lites et al., 2004; Jafarzadeh et al., 2017; Pietarila et al., 2009). In the new modified facula model, we use a different method to introduce force corrections into the potential distribution of the magnetic field, which causes the appearance of additional terms in the formulas for pressure and density. In the new version of the model, a change in only geometric parameters leads to a sharp change in the temperature profiles of the facular knot: instead of a dark central dip in the center of the assembly, a bright, hot formation can occur. An observational example of such a large-scale transformation is found in the Solar Dynamics Observatory data.

中文翻译：

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面KNOT的修改后的3D模型

摘要

本文介绍了先前发布的太阳太阳眼结的3D模型的修改版本（Solov'ev和Kirichek，2019），该模型成功描述了太阳太阳眼地层的主要结构特征。像在主模型中一样，我们使用电势逼近中的解（Schatzman，1965）作为流形单元磁性结构的基础。如前所述，光斑的磁轮廓具有喷泉的形状，其中稀薄的等离子体流在结点的中心上升，并沿磁场线在其外围流动。这种配置与观察到的模式非常相似（Lites等，2004; Jafarzadeh等，2017; Pietarila等，2009）。在新的改进的光斑模型中，我们使用另一种方法将力校正引入磁场的电势分布中，这导致在压力和密度公式中出现其他术语。在该模型的新版本中，仅几何参数的变化会导致球形结温度分布的急剧变化：可以在装配中心出现明亮的热变形，而不是在装配中心形成深色的中心倾角。在太阳动力学天文台的数据中找到了这种大规模变迁的观测示例。