Counter-streaming flows in a small (100" -long) solar filament/filament channel are directly observed in high-resolution SDO/AIA EUV images of a region of enhanced magnetic network. We combine images from SDO/AIA, SDO/HMI and IRIS to investigate the driving mechanism of these flows. We find that: (i) counter-streaming flows are present along adjacent filament/filament channel threads for about 2 hours, (ii) both ends of the filament/filament channel are rooted at the edges of magnetic network flux lanes along which there are impinging fine-scale opposite-polarity flux patches, (iii) recurrent small-scale jets (known as network jets) occur at the edges of the magnetic network flux lanes at the ends of the filament/filament channel, (iv) the recurrent network jet eruptions clearly drive the counter-streaming flows along threads of the filament/filament channel, (v) some of the network jets appear to stem from sites of flux cancelation, between network flux and merging opposite-polarity flux, and (vi) some show brightening at their bases, analogous to the base brightening in coronal jets. The average speed of the counter-streaming flows along the filament/filament channel threads is 70 km/s. The average widths of the AIA filament/filament channel and the Halpha filament are 4" and 2.5", respectively, consistent with the earlier findings that filaments in EUV images are wider than in Halpha images. Thus, our observations show that the continually repeated counter-streaming flows come from network jets, and these driving network-jet eruptions are possibly prepared and triggered by magnetic flux cancelation.
Imaging and Spectroscopic Observations of a Filament Channel and the Implications for the Nature of Counter-streamings
在2011年1月29日的暗条爆发之前和期间，利用成像和光谱望远镜观测暗条通道的动态。极紫外（EUV）光谱观测结果表明，在暗条通道中不存在H $α$逆流的EUV对应物，这意味着以往研究中发现的H $α$逆流主要是由于暗条通道中暗条线的纵向振荡引起的，它们之间并不同相.然而，存在较大规模的片状逆流EUV沿灯丝通道从一个极性到另一个，这意味着有另一个组件的单向流动（在$\pm$ 10 km s $^{-1}$的范围内）内的每个灯丝线程除了隐含的纵向振荡。我们的研究结果表明，在EUV的大规模斑片状逆流等离子体的流动方向有关的斑或活动网络的强度，与上升流位于较亮的区域的斑和下降流在较弱的地区。此外，我们提出了一种新的方法来确定的手征性的基础上的共轭细丝排水网站的偏斜爆发细丝。这表明，右偏排水对应于左旋手性，而左偏排水对应于右旋手性。
We analyze the high-resolution observations from the 1.6m telescope at Big Bear Solar Observatory that cover an active region filament. Counter-streaming motions are clearly observed in the filament. The northern end of the counter-streaming motions extends to a light bridge, forming a spectacular circulation pattern around a sunspot, with clockwise motion in the blue wing and counterclockwise motion in the red wing as observed in Halpha off-bands. The apparent speed of the flow is around 10 to 60 km/s in the filament, decreasing to 5 to 20 km/s in the light bridge. The most intriguing results…
A giant solar filament was visible on the solar surface from 2011 Nov. 8-23. The filament stretched over more than half a solar diameter. Multiwavelength data from the SDO instrument AIA (171, 193, 304, and 211Å) were used to examine counter-streaming flows within the spine of the filament. H$α$ images from the Kanzelhöhe Solar Observatory provided context information. We apply local correlation tracking (LCT) to a two-hour time series on 2011 Nov. 16 of the AIA images to derive horizontal flow velocities of the filament. To enhance the contrast of the AIA images, noise adaptive fuzzy equaliza…
Solar filaments exist as stable structures for extended periods of time before many of them form the core of a CME. We examine the properties of an erupting filament on 2017 May 29--30 with high-resolution He I 10830 A and Halpha spectra from the Dunn Solar Telescope, full-disk Dopplergrams of He I 10830 A from the Chromospheric Telescope, and EUV and coronograph data from SDO and STEREO. Pre-eruption line-of-sight velocities from an inversion of He I with the HAZEL code exhibit coherent patches of 5 Mm extent that indicate counter-streaming and/or buoyant behavior. During the eruption, indivi…
We report a detailed analysis of a failed eruption and flare in active region 12018 on 2014 April 3 using multiwavelength observations from SDO/AIA, IRIS, STEREO, and Hinode/SOT. At least four jets were observed to emanate from the cusp of this small active region (large bright point) with a null-point topology during the two hours prior to the slow rise of a filament. During the filament slow rise multiple plasma blobs were seen, most likely formed in a null-point current sheet near the cusp. The subsequent filament eruption, which was outside the IRIS field of view, was accompanied by a flar…
A giant quiescent solar filament observed with high-resolution spectroscopy
2011年11月15日，泰德天文台的真空塔望远镜用高分辨率的埃歇尔摄谱仪观测到了一个巨大的安静的太阳灯丝。在色球层吸收线H-α和Na I D2中同时记录了一组光谱（10张100”X 182”的图）。采用云模型（CM）反演和线芯拟合的灯丝等离子体的物理参数。光谱与色球望远镜（ChroTel）的全圆盘滤波图（He I 10830 A，H-α和Ca II K）和HMI的全圆盘磁图进行了补充。这条暗条有着极大的线性尺寸（817”），相当于太阳表面一个大圆上的658微米。使用CM方法反转总共175119个H-α对比度曲线。推断的平均视线（LOS）的速度，多普勒宽度，和源函数是类似于以前的作品较小的静态灯丝。然而，导出的光学厚度较大。从H-α线核心拟合推断的LOS速度趋势是一致的，但小于CM反演得到的。在灯丝中检测到逆流流动的特征。Na I D2线芯中最大的增亮聚集体与HMI所见的小尺度磁场吻合得很好。在倒刺末端附近检测到混合磁极性。根据HMI磁象图计算光球水平流，发现在暗条末端有大小为5-8 μ m、速度为0.30-0.45 km/s的流核。极大细丝的物理性质与其较小的对应物相似，除了在我们的样品中发现的光学厚度更大。我们发现，前一天爆发的一部分暗条正在重建其初始配置。
The fine dynamics in homologous and recurrent jets induced by persistent rising loops and mini-filaments
Institute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University（南京大学苏州校区深空探测科学与技术研究院）；State key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology（澳门科技大学月球与行星科学国家重点实验室）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；Yunnan Key Laboratory of Solar Physics and Space Science（云南省太阳物理与空间科学重点实验室）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education（教育部现代天文学与天体物理重点实验室（南京大学））
Supersonic flows observed by THEMIS related to a coronal bright point and filament
Kumaun University（库马翁大学）；Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Cité（巴黎天文台，巴黎文理研究大学，法国国家科学研究中心，索邦大学，巴黎西岱大学）；KU Leuven（荷语鲁汶大学）；University of Glasgow（格拉斯哥大学）；LUNEX EMMESI Institut（LUNEX EMMESI研究所）；University of Oslo（奥斯陆大学）；University of Maria Curie-Skłodowska（玛丽亚·居里-斯可洛多夫斯卡大学）
We present observations and modeling of the magnetic field configuration, morphology, and dynamics of a large-scale, high-latitude filament eruption observed by the Solar Dynamics Observatory. We analyze the 2015 July 9-10 filament eruption and the evolution of the resulting coronal mass ejection (CME) through the solar corona. The slow streamer-blowout CME leaves behind an elongated post-eruption arcade above the extended polarity inversion line that is only poorly visible in extreme ultraviolet (EUV) disk observations and does not resemble a typical bright flare-loop system. Magnetohydrodyna…
Solar Magnetized Tornadoes: Rotational Motion in a Tornado-like Prominence
Su等人在2012年提出了一种新的解释，认为细丝的形成和喷发是由表面上的漩涡驱动的旋转磁性结构。当这些结构出现在边缘上方时，它们被认为是类似龙卷风的风暴。它们可能作为等离子体的来源和细丝的扭曲起着关键作用。然而，没有观测成功区分旋转运动的磁结构在龙卷风般的湍流从其他运动，如振荡和逆流等离子体流。在这里，我们报告的证据旋转运动在一个龙卷风般的突出。两条日冕线的光谱观测是由一个专门设计的Hinode/EIS观测程序获得的。这些数据揭示了在日珥腿中存在冷的和百万度的热等离子体，支持所谓的“日冕过渡区”。日珥两侧相反的速度和它们持续的时间演化，以及SDO/AIA暗结构中明显的周期性运动，表明冷、热等离子体都有一个旋转运动，速度为$\sim$ 5 km s $^{-1}$ .
Solar coronal jets have been observed in detail since the early 1990s. While it is clear that these jets are magnetically driven, the details of the driving process has recently been updated. Previously it was suspected that the jets were a consequence of magnetic flux emergence interacting with ambient coronal field. New evidence however indicates that often the direct driver of the jets is erupting field, often carrying cool material (a "minifilament"), that undergoes interchange magnetic reconnection with preexisting field ([1]). More recent work indicates that the trigger for eruption of t…
Breakout/Interchange Reconnection as a driver of Jets, Fast Coronal Mass Ejection, and Solar Energetic Particles
American University（美国大学）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；University of California, Berkeley（加州大学伯克利分校）；Durham University（杜伦大学）；University of Michigan（密歇根大学）；The Catholic University of America（天主教大学）
