互联网区域磁性元素的日结观测
Hinode Observations of Magnetic Elements in Internetwork Areas
摘要：
我们使用序列的图像和磁图从日出研究磁性元素的互联网部分的安静的太阳光球。目视检查显示存在许多长寿命（几个小时）的结构，它们经常相互作用，并且可能在几个小时内迁移约7 Mm的距离。大约五分之一的元素在G带或Ca II H强度中具有相关的亮点。我们应用一个基于神经网络的算法来识别元素。该算法能够跟踪元素平均约10分钟。元素间歇性地下降到检测极限以下，尽管相关的通量显然持续存在，并且经常在一段时间后重新出现。我们从元素的连续位置推断出它们的自行，发现它们服从高斯分布，均方根为1.57 ± 0.08 km/s。表观流量表明，网络边界的偏差约为0.2公里/秒。负极性的元件显示出比正极性的元件更高的偏置，这可能是由于视场中网络的主导正极性，或者是由于它们的较小尺寸而增加的迁移率。在X轴上运动的偏好很可能是由该方向上更高的超颗粒流来解释的。我们通过将在空间和时间上看起来很接近的相反极性的元素分组来寻找新兴的两极。我们没有发现证据支持乔伊定律在弧秒尺度。
英文摘要：
We use sequences of images and magnetograms from Hinode to study magnetic elements in internetwork parts of the quiet solar photosphere. Visual inspection shows the existence of many long-lived (several hours) structures that interact frequently, and may migrate over distances ~7 Mm over a period of a few hours. About a fifth of the elements have an associated bright point in G-band or Ca II H intensity. We apply a hysteresis-based algorithm to identify elements. The algorithm is able to track elements for about 10 min on average. Elements intermittently drop below the detection limit, though the associated flux apparently persists and often reappears some time later. We infer proper motions of elements from their successive positions, and find that they obey a Gaussian distribution with an rms of 1.57+-0.08 km/s. The apparent flows indicate a bias of about 0.2 km/s toward the network boundary. Elements of negative polarity show a higher bias than elements of positive polarity, perhaps as a result of to the dominant positive polarity of the network in the field of view, or because of increased mobility due to their smaller size. A preference for motions in X is likely explained by higher supergranular flow in that direction. We search for emerging bipoles by grouping elements of opposite polarity that appear close together in space and time. We find no evidence supporting Joy's law at arcsecond scales.
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