发表机构
Institute of Science and Technology for Deep Space Exploration, Suzhou Campus, Nanjing University; Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education; Key Laboratory of Space Weather, National Satellite Meteorological Center (National Center for Space Weather), China Meteorological Administration; Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences; School of Astronomy and Space Science, University of Science and Technology of China; Innovation Center for FengYun Meteorological Satellite (FYSIC); School of Astronomy and Space Science, Nanjing University（南京大学苏州校区深空探测科学与技术研究院; 现代天文与天体物理教育部重点实验室（南京大学）; 中国气象局国家卫星气象中心（国家空间天气监测预警中心）空间天气重点实验室; 中国科学院紫金山天文台暗物质与空间天文重点实验室; 中国科学技术大学天文与空间科学学院; 风云气象卫星创新中心; 南京大学天文与空间科学学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
报道一个日珥未抛射的耀斑事件，通过多卫星观测和磁场外推，揭示自约束拉链式磁重联驱动耀斑并增强磁约束，阻止日珥抛射。
AI 中文摘要
对于与抛射日珥相关的耀斑，日珥通常上升至耀斑后环上方。本文报道了一个异常事件，其中耀斑后环反而覆盖了一个在整个耀斑期间保持非抛射状态的日珥。该事件由中国Hα太阳探测器（CHASE）、风云四号C星上的太阳极紫外成像仪（SUVI）、先进天基太阳天文台（ASO-S）上的硬X射线成像仪（HXI）以及太阳动力学天文台（SDO）同时捕获。FY4C/SUVI和SDO提供的极紫外（EUV）观测显示，耀斑开始时形成两个热环系统。北环系统的西端经历西南向漂移运动，剪切逐渐增大，而南环系统逐渐向北方汇聚并最终覆盖北环。同时，三维磁场外推揭示耀斑后支撑日珥的磁结构及其极向磁场均增强。综合这些观测，表明该耀斑由自约束拉链式磁重联驱动，其中高度剪切的弧状结构重联形成一系列上覆耀斑弧和底层磁通绳。这种重联不断增强对日珥的磁约束，阻止其向外抛射，同时促进沿重联磁场的大量等离子体排空，这由CHASE Hα光谱观测所揭示。
英文摘要
For flares associated with eruptive filaments, the filament normally rises above the post-flare loops. Here, we report an unusual event in which the post-flare loops instead overlie a filament that remains non-ejected throughout the flare. This event was simultaneously captured by the Chinese H$α$ Solar Explorer (CHASE), the Solar Extreme-UltraViolet Imager (SUVI) onboard Fengyun-4C, the Hard X-ray Imager (HXI) onboard the Advanced Space-based Solar Observatory (ASO-S) and the Solar Dynamics Observatory (SDO). Extreme Ultraviolet (EUV) observations provided by FY4C/SUVI and SDO show that two hot loop systems form at the flare onset. The western end of the northern loop system undergoes a southwestward drifting motion with gradually increasing shear, whereas the southern loop system progressively converges toward and eventually overlies the northern one. Meanwhile, three-dimensional magnetic field extrapolations reveal an increase in both the twist of the filament-supporting magnetic structure and its poloidal magnetic field after the flare. Taken together, these observations suggest that the flare is driven by a self-constraining zipper-type magnetic reconnection, in which highly sheared arcades reconnect to form a series of overlying flare arcades and an underlying flux rope. This reconnection continuously strengthens the magnetic confinement of the filament, preventing its outward eruption, while facilitating substantial plasma drainage along the reconnected magnetic field revealed by the CHASE H$α$ spectroscopic observations.
Comments13 pages, 5 figures, accepted for publication in ApJL
