IRIS观测到的亚巴秒亮点和静止暗条下的准周期上升流
Subarcsecond Bright Points and Quasi-periodic Upflows Below a Quiescent Filament Observed by the IRIS
摘要：
利用IRIS的紫外光谱和SJIs，以及太阳动力学天文台（SDO）的日冕图像和磁图，我们提出了一个静止的暗条通道的新特征：亚弧秒亮点（BPs）和准周期上升流。TR中的BP具有约350 $-$ 580 km的空间尺度和超过几十分钟的寿命。它们位于细丝通道中较强的磁性结构处，磁通量约为10 $^{17}$ $-$ 10 $^{18}$ Mx。准周期性的增亮和上升流中观察到的BP和周期约为4 $-$ 5分钟。BP和相关的射流状上升流包括一个“蝌蚪形”的结构。上升流沿明亮的细丝运动，其方向几乎平行于细丝的脊。从具有相反极性磁场的BPs发起的上升流具有相反的方向。上升气流在天空平面内的速度约为5 $-$ 50 km s $^{-1}$。Si IV 1402.77的发射线在上升流处出现了约5 $-$ 30 km s $^{-1}$的明显蓝移，谱线轮廓展宽，宽度超过20 km s $^{-1}$。这些边界点似乎是细丝的基础，并且上升流能够输送质量以实现细丝的动态平衡。先前观测中的“逆流”流动可能是由相反极性磁场引发的双向上升流的传播引起的。我们认为，准周期性增亮的BPs和准周期性上升流的小尺度振荡的磁重联，这是由太阳p模式波调制的结果。
英文摘要：
Using UV spectra and SJIs from the IRIS, and coronal images and magnetograms from the Solar Dynamics Observatory (SDO), we present the new features in a quiescent filament channel: subarcsecond bright points (BPs) and quasi-periodic upflows. The BPs in the TR have a spatial scale of about 350$-$580 km and lifetime of more than several tens of minutes. They are located at stronger magnetic structures in the filament channel, with magnetic flux of about 10$^{17}$$-$10$^{18}$ Mx. Quasi-periodic brightenings and upflows are observed in the BPs and the period is about 4$-$5 min. The BP and the associated jet-like upflow comprise a "tadpole-shaped" structure. The upflows move along bright filament threads and their directions are almost parallel to the spine of the filament. The upflows initiated from the BPs with opposite polarity magnetic fields have opposite directions. The velocity of the upflows in plane of sky is about 5$-$50 km s$^{-1}$. The emission line of Si IV 1402.77 Å at the locations of upflows exhibits obvious blueshifts of about 5$-$30 km s$^{-1}$, and the line profile is broadened with the width of more than 20 km s$^{-1}$. The BPs seem to be the bases of filament threads and the upflows are able to convey mass for the dynamic balance of the filament. The "counter-streaming" flows in previous observations may be caused by the propagation of bi-directional upflows initiated from opposite polarity magnetic fields. We suggest that quasi-periodic brightenings of BPs and quasi-periodic upflows result from small-scale oscillatory magnetic reconnections, which are modulated by solar p-mode waves.
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