在非常安静的阳光下，
Dead calm areas in the very quiet Sun
摘要：
我们分析了“日出”号气球上搭载的IMaX偏振分光仪在高空间分辨率（~100 km）下观测到的两个宁静太阳区域（35.6 x 35.6 Mm^2）的偏振光。我们确定了497个小尺度（~400 km）的磁环，其有效速率为0.25圈h^{-1} arcsec^{-2};此外，我们认为这个数字和速率被低估了~ 30%。然而，我们发现这些小偶极子并不均匀地出现在太阳表面上：它们的空间分布是相当复杂和混乱的，创造了死平静的区域，其特征是非常低的磁信号和缺乏有组织的环状结构，在我们的仪器的检测水平上，这不能被解释为泊松空间过程的统计波动。我们认为，这是在非常安静的太阳产生磁场的机制的内在特征。这种现象的时空相干性和星团结构表明，在太阳最安静的区域产生磁场的机制是周期性的、间歇性的。
英文摘要：
We analyze two regions of the quiet Sun (35.6 x 35.6 Mm^2) observed at high spatial resolution (~100 km) in polarized light by the IMaX spectropolarimeter onboard the Sunrise balloon. We identify 497 small-scale (~400 km) magnetic loops, appearing at an effective rate of 0.25 loop h^{-1} arcsec^{-2}; further, we argue that this number and rate are underestimated by ~30%. However, we find that these small dipoles do not appear uniformly on the solar surface: their spatial distribution is rather filamentary and clumpy, creating dead calm areas, characterized by a very low magnetic signal and a lack of organized loop-like structures at the detection level of our instruments, that cannot be explained as just statistical fluctuations of a Poisson spatial process. We argue that this is an intrinsic characteristic of the mechanism that generates the magnetic fields in the very quiet Sun. The spatio-temporal coherences and the clumpy structure of the phenomenon suggest a recurrent, intermittent mechanism for the generation of magnetic fields in the quietest areas of the Sun.
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