标题： 太阳内部网络。 III. 单极与双极磁通出现 显示英文标题

标题： The solar internetwork. III. Unipolar versus bipolar flux appearance

摘要： 小尺度内联网（IN）磁场被认为是宁静太阳磁性的主要构建块。 因此，了解它们如何出现在太阳表面上至关重要。 在此，我们采用高分辨率、高灵敏度、长时间的Hinode/NFI磁图序列，分析超granular细胞中心内部单个IN磁场元素的出现模式和时空演化。 通过通量斑块的识别和磁摩擦模拟，我们表明IN通量浓度存在两种不同的群体：单一极性和双极性特征。 双极性特征通常比单一极性特征更大更强。 它们寿命更长，每个特征携带的通量更多。 这两种类型的通量浓度在太阳表面上均匀出现。 然而，我们认为双极性特征真正代表了新通量在太阳表面的浮现，而单一极性特征似乎是由背景通量的合并形成的。 双极性特征的出现速度比单一极性特征快（68 对 55 Mx cm$^{-2}$天$^{-1}$），并且提供约70%在超granule内部检测到的总瞬时IN通量。 显示英文摘要

摘要： Small-scale internetwork (IN) magnetic fields are considered to be the main building blocks of the quiet Sun magnetism. For this reason, it is crucial to understand how they appear on the solar surface. Here, we employ a high-resolution, high-sensitivity, long-duration Hinode/NFI magnetogram sequence to analyze the appearance modes and spatio-temporal evolution of individual IN magnetic elements inside a supergranular cell at the disk center. From identification of flux patches and magnetofrictional simulations, we show that there are two distinct populations of IN flux concentrations: unipolar and bipolar features. Bipolar features tend to be bigger and stronger than unipolar features. They also live longer and carry more flux per feature. Both types of flux concentrations appear uniformly over the solar surface. However, we argue that bipolar features truly represent the emergence of new flux on the solar surface, while unipolar features seem to be formed by coalescence of background flux. Magnetic bipoles appear at a faster rate than unipolar features (68 as opposed to 55 Mx cm$^{-2}$ day$^{-1}$), and provide about 70% of the total instantaneous IN flux detected in the interior of the supergranule.