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感应暗条爆发物理机制研究
其他题名Formation Mechanism of Sympathetic Filament Eruption
周承瑞
学位类型硕士
导师申远灯
2022-07-01
学位授予单位中国科学院大学
学位授予地点北京
培养单位中国科学院云南天文台
学位专业天体物理
关键词太阳耀斑 暗条 太阳磁场 太阳活动
摘要太阳是我们唯一一颗能够清楚观测到的恒星,其每时每刻都在发出着极其 丰富的能量,在太阳大气中充满着各种各样的活动,比如太阳耀斑、太阳喷流、 太阳风、暗条爆发、日冕物质抛射、大尺度极紫外 (EUV) 波等。地球上绝大部分 能量也来自太阳,太阳爆发活动与地球息息相关,例如:太阳发射的高能粒子到 达地球可以形成美丽的极光,而太阳上的各种爆发也是地球上灾难性空间天气 的主要来源。因此研究太阳爆发活动的形成和演化的物理机制,以期对其进行准 确预报,对地球有着极为重要的意义。太阳暗条的爆发又作为空间天气的主要物 质来源,其爆发机制和模式被研究人员广泛研究。其中的感应暗条爆发模式,在 最近也越来越引起了研究人员的关注。在感应暗条爆发方面,目前还不清楚在很短时间内不同地点的连续暗条爆 发是否具有物理联系。为了解释这部分疑惑,我们研究了一个位于三极磁场的连 续小暗条和大暗条爆发的感应暗条爆发事件,该区域的日冕磁场显示为一个扇 面脊磁系统。我们分析了 X 射线波段与极紫外波段的观测数据,并使用 HMI 矢 量磁场数据做非线性无力场外推得到的三维日冕磁场,我们发现这两个暗条分 别扎根于扇面脊磁系统内部扇形结构的两个腔内。此外,挤压因子图还显示了一 个位于大扇形脊系统的扇形结构的东叶的小扇面脊系统。通过观测,我们发现小 暗条的爆发是一次失败的爆发,除了三个耀斑带和内外重联引起的耀斑后环外, 没有引起任何日冕物质抛射(CME)。大暗条的爆发不仅引起了类似于小暗条爆 发中观察到的耀斑后环和耀斑带,还引起了大尺度的 CME。根据我们的分析结 果,我们得出结论,这两次连续的暗条爆发是有物理联系的,其中小暗条爆发引 起的日冕磁场的磁拓扑结构变化被认为造成此次感应暗条爆发的原因。此外,研 究结果还表明,小扇面脊结构的爆发进一步加速了大暗条的不稳定和爆发。目前人们对太阳相应暗条活动的物理形成和演化规律还不太清楚,许多谜 团的揭开还需要依赖未来更高分辨率观测数据和更多的模拟工作的进展。
其他摘要The solar is the only star that we can easily observe, it emitted abundance of its energy, which includes full of various activities such as solar flares, solar jets, solar winds, filament eruption, coronal mass ejections, and large scale extreme ultraviolet (EUV) waves. The vast majority of energy on earth comes from the solar, and solar eruptive activities are closely related to the safe of earth. eg, High-energy particles emitted by the solar can reach the earth to form beautiful auroras, and the eruption on the solar are the main source of catastrophic space weather on earth. In older to forecast them accurately, it is of great importance for the earth to study the physical mechanisms of solar activity. The eruption of the filament on the sun are the main material source of space weather, and their eruption mechanisms have been widely studied by researchers. The physical linkage of the sympathetic filament eruption has also attracted the researchers, recently. It is unclear whether successive filament eruptions at different sites within a short time interval are physically connected or not. Here, we present the observations of suc- cessive eruptions of a small and a large filament in a tripolar magnetic field region whose coronal magnetic field showed as a fan-spine magnetic system. By analyzing the multi-wavelength observations taken by the Solar Dynamic Observatory and the extrapolated three-dimensional coronal magnetic field, we find that the two filaments resided respectively in the two lobes that make up the inner fan structure of the fan-spine magnetic system. In addition, a small fan-spine system was also revealed by the squashing factor Q map, which located in the east lobe of the fan structure of the large fan-spine system. The eruption of the small filament was a failed filament eruption, which did not cause any coronal mass ejection (CME) except for three flare ribbons and two post-flare-loop systems connecting the three magnetic polarities. The eruption of the large filament not only caused similar post-flare-loop systems and flare ribbons, as observed in the small filament eruption, but also a large-scale CME. Based on our analysis results, we conclude that the two successive filament eruptions were physically connected, in which the topology change caused by the small filament eruption is thought to be the physical linkage. In addition, the eruption of the small fan-spine structure further accelerated the instability and violent eruption of the large filament. Lots of solar activities still remain unsolved. To find the answers out, we may need hegher resolution solar telescopes and simulations.
学科领域天文学 ; 太阳与太阳系 ; 太阳物理学
学科门类理学 ; 理学::天文学
页数0
语种中文
文献类型学位论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/25770
专题选址与日冕观测组
推荐引用方式
GB/T 7714
周承瑞. 感应暗条爆发物理机制研究[D]. 北京. 中国科学院大学,2022.
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