太阳能互联网II。磁通量出现率和消失率
The Solar Internetwork. II. Magnetic Flux Appearance and Disappearance Rates
摘要：
小规模互联网络磁场是宁静太阳的重要组成部分。在本文中，我们分析了它们如何出现和消失在太阳表面。使用高分辨率的Hinode magnetograms，我们遵循在磁盘中心的两个超颗粒细胞内部的个别磁性元素的演变。从长达38小时的连续测量，我们表明，磁通量出现在互联网区域的速度$120\pm3$ Mx厘米$^{-2}$天$^{-1}$（$3.7 \pm 0.4 \times 10^{24}$ Mx天$^{-1}$在整个太阳表面）。磁通量以$125 \pm 6$ Mx cm $^{-2}$ day $^{-1}$（$3.9\pm 0.5 \times 10^{24}$ Mx day $^{-1}$）的速率从互联网络中消失，这是通过磁性元素的衰落、相反极性特征之间的抵消以及与网络补丁的相互作用实现的，网络补丁将互联网络元素转换为网络特征。大部分通量通过衰落和与网络的相互作用而损失，几乎以大约50 Mx cm $^{-2}$天$^{-1}$的速率损失。我们的结果表明，互联网络的磁通量的源和汇是很好的平衡。利用瞬时通量的出现和消失率，我们成功地再现了两个超颗粒细胞的总无符号通量的时间演化。
英文摘要：
Small-scale internetwork magnetic fields are important ingredients of the quiet Sun. In this paper we analyze how they appear and disappear on the solar surface. Using high resolution Hinode magnetograms, we follow the evolution of individual magnetic elements in the interior of two supergranular cells at the disk center. From up to 38 hr of continuous measurements, we show that magnetic flux appears in internetwork regions at a rate of $120\pm3$ Mx cm$^{-2}$ day$^{-1}$ ($3.7 \pm 0.4 \times 10^{24}$ Mx day$^{-1}$ over the entire solar surface). Flux disappears from the internetwork at a rate of $125 \pm 6$ Mx cm$^{-2}$ day$^{-1}$ ($3.9\pm 0.5 \times 10^{24}$ Mx day$^{-1}$) through fading of magnetic elements, cancellation between opposite-polarity features, and interactions with network patches, which converts internetwork elements into network features. Most of the flux is lost through fading and interactions with the network, at nearly the same rate of about 50 Mx cm$^{-2}$ day$^{-1}$. Our results demonstrate that the sources and sinks of internetwork magnetic flux are well balanced. Using the instantaneous flux appearance and disappearance rates, we successfully reproduce the time evolution of the total unsigned flux in the two supergranular cells.
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