Prominence plumes are evacuated upflows that emerge from bubbles below prominences, whose formation mechanism is still unclear. Here we present a detailed study of plumes in a quiescent prominence using the high-resolution H-alpha filtergrams at the line center as well as line wing at +/-0.4 angstrom from the New Vacuum Solar Telescope. Enhancements of brightening, blue shifts, and turbulence at the fronts of plumes are found during their formation. Some large plumes split at their heads and finger-shaped structures are formed between them. Blue-shifted flows along the bubble-prominence interface are found before and during the plume formation. Our observations are consistent with the hypothesis that prominence plumes are related to coupled Kelvin-Helmholtz and Rayleigh-Taylor (KH/RT) instabilities. Plume splittings and fingers are evidence of RT instability, and the flows may increase the growth rate of KH/RT instabilities. However, the significant turbulence at plume fronts may suggest that the RT instability is triggered by the plumes penetrating into the prominence. In this scenario, extra mechanisms are necessary to drive the plumes.
To understand the formation mechanism of large plumes in solar prominences, we investigate the formation process of two such phenomena. We studied the dynamic and thermal properties of two large plumes using observations from New Vacuum Solar Telescope, the Solar Dynamic Observatory, and the Solar Terrestrial Relations Observatory-Ahead. We find that two large plumes observed with high-resolution data are quite different from previously studied small-scale plumes. They are born at the top of a prominence bubble with a large projected area of 10-20 Mm^2 . Before the occurrence of each large plu…
Time evolution of plasma parameters during the rise of a prominence instability
我们提出了高空间分辨率的光谱偏振观测的一个静止的树篱日珥在他我1083.0 nm的三重态。观察包括一个时间序列，在坐和盯着模式的36分钟的持续时间。摄谱仪的狭缝穿过日珥主体，我们记录了单个垂直线的时间演化。最终，我们观察到一个黑暗的瑞利-泰勒羽状物的发展，它以17公里/秒的速度向上传播，投射到天空平面上。有趣的是，烟羽的顶点与日珥的丝线相撞，将它们推向一边。我们通过使用HAZEL代码解释He I Stokes剖面来推断多普勒频移、多普勒宽度和磁场强度变化。多普勒频移表明，线程集群一致地移动，而个别线程有振荡模式。关于羽流，我们发现了强烈的红移（9-12公里/秒）和大的多普勒宽度（10公里/秒），在羽流的顶点时，它通过突出的身体和解体之前。我们将红移与透视效应联系起来，而多普勒宽度更可能是由于局部温度的增加。没有发现与羽流通过相关的磁场强度的局部变化;这使我们得出结论，羽流并不比周围环境更磁化。最后，我们发现，一些线程振荡是局部阻尼，这使我们能够应用日珥地震学技术来推断额外的日珥物理参数。
Statistical Study of Solar Prominence Plumes Based on NVST H$α$ Observations
School of Physical Science and Technology, Southwest Jiaotong University（西南交通大学物理科学与技术学院）；National Astronomical Observatories, Chinese Academy of Science（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；Yunnan Observatories, Chinese Academy of Sciences（中国科学院云南天文台）；National Space Science Center, Chinese Academy of Sciences（中国科学院国家空间科学中心）；North China University of Technology（华北理工大学）；Beijing Planetarium, Beijing Academy of Science and Technology（北京天文馆（北京市科学技术研究院））
Measuring vector magnetic fields in solar prominences
我们目前的分光偏振观测在他我1083.0 nm多重的一个静止的，树篱日珥。这些数据是用特内里费岛红外线偏振计拍摄的，该偏振计安装在位于西班牙加那利群岛特内里费岛天文台（Observatorio del Teide）的德国真空塔望远镜上。所观察到的He I圆偏振和线偏振信号分别由塞曼效应和原子级偏振和汉勒效应主导。这些可观测量对视场的每个空间点处的磁场矢量的强度和方向敏感。我们确定的磁场矢量的日珥应用HAZEL反演代码所观察到的斯托克斯轮廓。我们简要讨论了检索的磁场矢量配置。
A first look into the magnetic field configuration of prominence threads using spectropolarimetric data
我们显示了一个正在进行的调查，旨在确定配置的磁场向量的线程的一个静止的树篱日珥使用高空间分辨率的分光偏振观测在He I 1083.0 nm多重。数据包括一个静态的树篱日珥显示垂直线程的二维地图。这些观测是用特内里费岛红外线偏振计获得的，该偏振计安装在位于西班牙天文台的德国真空塔望远镜上。He I 1083.0 nm斯托克斯信号解释与反转码，它考虑到关键的物理过程，产生和/或修改圆和线性偏振信号在He I 1083.0 nm三重态：塞曼效应，各向异性辐射泵浦，和汉勒效应。我们目前的反演，即沿日珥和日珥线程的磁场矢量的强度和方向的初步结果。
The Spontaneous Genesis of Solar Prominence Structures Driven by Supergranulation in Three-Dimensional Simulations
School of Physics and Astronomy, Yunnan University（云南大学物理与天文学院）；Yunnan Key Laboratory of Solar Physics and Space Science（云南太阳能物理与空间科学重点实验室）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）
The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He I 10830 A triplet
内容：通过解释谱线中的汉勒效应和塞曼效应，可以确定静止太阳黑子中的磁场矢量。然而，观测测量是稀缺的，缺乏高空间分辨率。目的：通过解释安装在泰德天文台的德国真空塔望远镜上的特内里费红外偏振计获得的He I 1083.0 nm三重态的分光偏振测量，确定沿静止日珥的磁场矢量配置。方法. He I 1083.0 nm三重态Stokes分布进行了分析，考虑到在这三重态的偏振信号的物理负责的反演代码。借助太阳动态观测台和日地关系观测台卫星进行的极紫外线观测，将结果纳入太阳背景。结果：对于最可能的磁场矢量配置，分析描绘了7高斯的平均场强。我们没有发现磁场强度的局部变化，只是平均而言，日珥体中的磁场强度低于日珥脚中的磁场强度，日珥脚中的磁场强度达到25高斯。相对于局部垂直线的平均磁场倾斜度为77度。磁场矢量与日珥主轴的锐角在左旋手征情况下为24度，在右旋手征情况下为58度。这些推论是在粗略的协议与以前的结果从较低的空间分辨率获得的数据分析。
The 2008 August 1 Eclipse Solar-Minimum Corona Unraveled
我们讨论的白光和[Fe XIV]发射日冕观测期间的日全食2008年8月1日，在蒙古（Altaj地区）和俄罗斯（Akademgorodok，新西伯利亚，西伯利亚）的结果。对应于目前的极端太阳极小期，白光日冕，可见达20个太阳半径，是一个短暂的类型与明显的头盔流光位于一个位置角48，130，241和322度的双折射链上方。在两极周围可以看到各种各样的冕洞，里面充满了一些细小的极地羽流。进一步的原始方法的图像处理，恒星高达12等，一个克鲁兹族彗星（C/2008 O 1），和一个日冕物质抛射（CME）也被检测到，与最小的可分辨的结构是，在某些地方甚至小于1角秒。即使我们的站点之间有19分钟的时间差，也可以看到日冕和日冕中的差异，可能是运动。除了显示连续日冕的高分辨率日冕图像外，（K-日冕），由光球光的电子散射产生，重叠的绿色发射线的图像（530.3nm，[Fe XIV]）电晕，并利用两个窄带滤光片进行了研究（分别以线本身为中心和对于529.1nm附近的连续谱），每个具有0.15nm的FWHM。通过太阳观测，我们咨询了太阳和日光层天文台，Hinode的XRT和SOT，TRACE和STEREO，以及Wilcox太阳天文台和SOHO/MDI磁图，我们将我们的日食观测放在当前异常低和延长的太阳极小期的背景下。
Dynamic features, such as chromospheric jets, transition region network jets, coronal plumes and coronal jets, are abundant in the network regions of the solar polar coronal holes. We investigate the relationship between chromospheric jets and coronal activities (e.g., coronal plumes and jets).We analyze observations of a polar coronal hole including the filtergrams that were taken by the New Vacuum Solar Telescope (NVST) at the Hα-0.6 Åto study the Hα jets,and the Atmospheric Imaging Assembly (AIA) 171 Å images to follow the evolution of coronal activities. Hα jets are persistent in the netwo…
The Multichannel Subtractive Double Pass (MSDP) is an imaging spectroscopy technique, which allows observations of spectral line profiles over a 2D field of view with high spatial and temporal resolution. It has been intensively used since 1977 on various spectrographs (Meudon, Pic du Midi, the German Vacuum Tower Telescope, THEMIS, Wrocław). We summarize previous developments and describe the capabilities of a new design that has been developed at Meudon and that has higher spectral resolution and increased channel number: Spectral Sampling with Slicer for Solar Instrumentation (S4I), which c…
The Hα spectral line is a well-studied absorption line revealing properties of the highly structured and dynamic solar chromosphere. Typical features with distinct spectral signatures in Hα include filaments and prominences, bright active-region plages, superpenumbrae around sunspots, surges, flares, Ellerman bombs, filigree, and mottles and rosettes, among others. This study is based on high-spectral resolution Hα spectra obtained with the echelle spectrograph of the Vacuum Tower Telescope (VTT) located at Observatorio del Teide (ODT), Tenerife, Spain. The t-distributed Stochastic Neighbor Em…
