太阳暗条的演化和爆发的系统研究

The filament is one of the most significant activities in solar physics. To study it can help us to totally understand all the solar activities. Employing the data of several satellites, e.g. the SDO, and some Earth-based telescopes, e.g. the NVST at Yunnan Astronomical Observatory (YNAO), we choose all filament observations as our sample. Using both case study and statistical study methods, and considering some empirical and theoretical models, we analyze the filaments, including their structures, evolutions, and eruptions. (1) The filament fine structures and their distributions, and also the distributions and evolution of photospheric magnetic fields are investigated. Considering some theoretical studies, we suggest the magnetic structures of filaments. The kinematic evolutions of filaments are investigated, such as the oscillation and flow. Analyzing the evolutions of both surrounding activities and magnetic fields, we study the physical causes of the kinematics of filaments. (2) Investigating the variations of the filaments and their surrounding structures before the filament eruptions, e.g. evolutions of nearby coronal loops or multi-wavelength emissions, we search for the pre-eruption activities. The brightening propagation of footpoints of erupting filaments is studied. Employing the magnetograms, we analyze the magnetic field distributions of these footpoints, and propose the physical mechanism of this propagation. We investigate the initial process of filament eruptions, and also the evolution of magnetic fields. The eruption physical mechanisms and initial erupting process are then proposed. The role of magnetic reconnection plays in the filament eruptions is also suggested. (3) We study the interaction between the erupting filaments and other surrounding coronal structures. The ways of interaction are established, and the physical nature is proposed. Investigating the spatial-temporal evolutions of filament eruptions and other associated activities, such as the flares, CMEs, and extreme-ultraviolet waves, we study the relationships among these activities. After finishing these investigations mentioned above, we would further understand the physical nature of the filaments, and also all the other associated activities.

暗条是太阳物理中至关重要的活动之一,对它的研究将帮助我们全面理解太阳爆发活动现象。使用SDO等卫星和云台NVST等望远镜的数据,我们筛选暗条观测,构建研究样本,结合个例和统计分析,参照经验和理论模型,系统研究暗条的结构、演化和爆发等。(1)分析暗条的精细纤维结构及其组成方式,和光球磁场的分布及演化,探讨暗条的磁结构;研究暗条的动力学演化,如振荡和流动等,及其周边的活动,探讨其物理成因。(2)分析暗条爆发前的活动,如冕环和多波段辐射等的变化,探寻爆发的前兆;研究暗条足点在爆发过程中的增亮传播,探讨其物理原因;研究暗条爆发的过程和磁场的演化,讨论暗条爆发的触发机制和初发过程，明确磁重联在暗条爆发中的作用。(3)分析爆发暗条与周边磁结构的相互作用,建立相互作用模式,探讨其物理原因;构建暗条爆发和耀斑、日冕物质抛射及波等相关活动的关系。通过上述研究,我们将进一步理解暗条本质,以及其他相关爆发活动。

太阳暗条（日珥）是一种悬浮于高温稀疏的日冕中低温致密的等离子体结构。它的爆发与耀斑、日冕物质抛射和喷流等活动密切相关，是灾害性空间天气扰动的日面来源。对它进行研究将帮忙我们更好地理解暗条，进而更好地预报空间天气。在本项目的支持下，项目组在暗条的形成、结构、演化和爆发等方面进行了全面系统的研究，在耀斑和喷流等相关活动的研究方面也取得了重要进展。.项目组和我们的合作者一起，使用多波段观测，发现了一种新的短时暗条的形成机制，提出了一种新的冕雨形成模型。我们指出，开放磁结构与其下方的闭合冕环之间的交换磁重联是形成短时暗条，以及后续冕雨的原因。.我们还分析了暗条结构及其演化，发现了暗条-日冕过渡区内的针状物和龙卷风暗条中的迷你喷流；研究了由两条具有不同手征性的暗条通道组成的一条巨型暗条通道；报道了一种新的色球扇形活动现象。.我们还系统研究了暗条爆发，报道了爆发暗条的解扭缠运动和两个暗条之间的感应爆发；分析了爆发暗条上方和下方的磁重联；研究了暗条爆发引起的龙卷风、传播的扭折波和耀斑等；分析了爆发暗条与扇-脊磁结构之间的相互作用，指出迷你暗条爆发是引起圆形耀斑的原因。.我们还研究了磁重联机制，分析了小尺度重联事件的光谱和图像特征；发现黑子半影暗条侵入亮桥触发了重联喷流，指出重联喷流是亮墙的组成部分；报道了活动区浮现初期的交换磁重联；提出两个磁系统之间的滑动磁重联是引起约束耀斑的原因。.我们还归纳出两类束缚耀斑；发现了活动区总磁通量是决定大耀斑是否束缚的重要因素；指出复杂磁结构之间的磁重联是引起束缚耀斑的原因；报道了耀斑带之间的相互碰撞；用深度学习的方法，用视向磁图预报耀斑。.我们还报道了由碰撞激发的表观扇形喷流和耀斑带上的喷流；研究了喷流过程中的磁流体不稳定性；通过分析沿环传播的物质流，研究了冕环的物理性质。.在本项目的支持下，我们已发表SCI论文33篇。在项目执行期间，两名研究生分别获得了博士和硕士学位。