鱼骨状结构中的连续磁重联导致的反复增亮现象
Sequential Magnetic Reconnections in a Fishbone-like Structure Leading to Recurrent Brightenings
浏览论文内容
中文总结 AI 辅助
本研究利用多卫星观测数据，揭示活动区12297内鱼骨状磁结构的连续磁重联导致反复增亮，深化了对太阳大气磁自由能精细耗散的理解。
中文摘要 AI 辅助
太阳大气中磁自由能的精细释放是太阳物理学中一个基本的开放问题，高时空分辨率的多波段观测为该过程提供了直接观测窗口。利用NVST、SDO、IRIS和Hinode的数据，我们揭示了活动区12297内一个鱼骨状磁结构的能量释放过程。该鱼骨状结构由一条沿狭窄、拉长的正极性磁场分布的脊线，以及扎根于负极性黑子的人字形分支组成。在该鱼骨状结构下方观测到持续的光球磁通量浮现和剪切运动，这可能在维持其拓扑结构和产生反复增亮中起到关键作用。增亮期间，紧凑的亮特征沿脊线从西向东连续传播，伴随分支上的双向流和向远处正极性黑子喷射的等离子体团。这些传播特征可被解释为沿脊线节点按时间顺序发生的连续磁重联事件的信号，这些事件主要发生在色球层和过渡区。我们的观测可能提供证据表明，反复增亮可由连贯磁结构组织的重复连续重联事件产生，加深了我们对这类反复增亮如何形成以及太阳活动区中磁自由能如何在精细尺度耗散的理解。
英文摘要
The fine-scale release of magnetic free energy in the solar atmosphere is a fundamental open question in solar physics. Multi-wavelength observations at high spatiotemporal resolution now offer a direct window into this process. Using data from NVST, SDO, IRIS, and Hinode, we reveal the energy release process in a fishbone-like magnetic structure within active region 12297. The fishbone-like structure consists of a spine along a narrow, elongated positive-polarity field, with herringbone branches rooted in negative-polarity sunspots. Persistent photospheric magnetic flux emergence and shearing motions are observed beneath the fishbone-like structure, which may play a key role in maintaining its topology and producing the recurrent brightenings. During brightenings, compact bright features propagate sequentially from west to east along the spine, accompanied by bidirectional flows along the branches and plasma blobs ejected toward the distant positive sunspot. These propagating features could be interpreted as signatures of sequential magnetic reconnection events occurring in chronological order at nodes along the spine, predominantly in the chromosphere and transition region. Our observations may provide evidence that recurrent brightenings could arise from repeated sequential reconnection events organized by a coherent magnetic structure, deepening our understanding of how such recurrent brightenings are generated and how magnetic free energy is dissipated at fine scales in solar active regions.
