发表机构
Patna University; National Institute of Technology Calicut; Indian Institute of Astrophysics（巴特那大学; 卡利卡特国家技术学院; 印度天体物理研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文利用SDO和Aditya-L1数据及NFFF外推，研究了X1.8耀斑的触发及准周期脉动，发现磁通量绳、3D零点等特征及其重复磁重联是关键。
AI 中文摘要
本文旨在探索X1.8级太阳耀斑（SOL2024-10-09T0124）的触发机制及其相关的准周期脉动（QPPs），该耀斑位于NOAA活动区13848内。为此，我们利用太阳动力学天文台（SDO）和Aditya-L1的数据对该事件进行了多波长分析。重要的是，观测表明在耀斑开始时出现了S形增亮，同时在耀斑峰值时间附近，耀斑增亮和耀斑带的复杂形态逐渐演化。此外，在耀斑的脉冲相期间检测到了QPPs，在硬X射线光变曲线中显示出约4分钟的主导周期。为了理解耀斑的触发机制，我们使用非无力场（NFFF）外推模型构建了耀斑前阶段的日冕磁场。外推的磁场揭示了耀斑区域内存在各种重要的磁特征，包括磁通量绳、三维（3D）零点、剪切弧状结构以及准分离层（QSLs）。这些特征处发生的重复磁重联被认为在耀斑的触发以及相关的QPPs中发挥作用。
英文摘要
The paper seeks to explore the initiation of an X1.8 class solar flare (SOL2024-10-09T0124) and the related quasi-periodic pulsations (QPPs), which are situated within NOAA active region 13848. To achieve this, we perform a multi-wavelength analysis of the event utilizing data from the Solar Dynamic Observatory (SDO) and Aditya-L1. Importantly, the observations indicate the emergence of a sigmoidal brightening at the onset of the flare, alongside the evolution of a complex morphology of flare brightenings and ribbons around the peak time of the flare. Furthermore, QPPs are detected during the impulsive phase of the flare, exhibiting a dominant period of approximately 4 minutes in the hard X-ray light curve. In order to comprehend the initiation of the flare, we construct the coronal magnetic field at a pre-flare stage by employing the non-force-free-field (NFFF) extrapolation model. The extrapolated magnetic field illustrates the existence of various significant magnetic features, including a magnetic flux rope, a three-dimensional (3D) null, sheared arcade, and quasi- separatrix layers (QSLs) within the flaring region. The recurrent reconnection occurring at these features is proposed to play a role in the initiation of the flare as well as the associated QPPs.
Comments21 pages, 9 figures accepted for publication in Solar Physics
