AI 中文总结
研究脉冲受限C级太阳耀斑，利用多波长数据集及非线性无力场外推，分析热等离子体与非热电子耦合、电子加速过程，探讨耀斑爆发与磁结构关系，解释非热发射中的非平稳准周期脉动。
AI 中文摘要
本文详细分析了脉冲C2.8太阳耀斑SOL2023-03-19T02:12，聚焦于微波和X射线领域。该耀斑因其脉冲性质、母活动区相对简单的磁形态、受限演化、中等强度、明显的非平稳时间行为以及独特多波长数据集的可用性而被选中。数据集包括用新的太阳射电光谱偏振仪获得的2.8-12GHz频率范围内的微波光谱观测以及西伯利亚射电日像仪的微波图像，还有两台成像X射线望远镜的观测。利用非线性无力场外推重建活动区的三维磁结构。在初始耀斑阶段，给出了热等离子体和非热电子群体在无碰撞等离子体框架内直接耦合的证据，并讨论了电子加速过程的一些简单关系。对推断磁场的分析表明耀斑爆发与沿极性反转线的低海拔剪切磁环系统有关。鉴于事件的受限性质和重建的磁结构，推断磁重联很可能发生在具有大量引导场分量的电流片中。在非热发射中观测到的非平稳准周期脉动，周期从约15秒降至9秒，被解释为在不同磁结构中发生的一系列磁重联事件的特征，由一个仍不确定但可能涉及传播慢磁声波的过程准周期触发。
英文摘要
A detailed analysis of the impulsive C2.8 solar flare SOL2023-03-19T02:12 is presented, focusing on the microwave (MW) and X-ray domains. The flare was selected because of its impulsive nature, the relatively simple magnetic morphology of its parent active region (AR) NOAA 13256, its confined evolution, its moderate intensity, pronounced non-stationary temporal behaviour, and the availability of a unique multi-wavelength dataset. This dataset includes MW spectral observations in the frequency range 2.8-12 GHz obtained with the new Solar Radio Spectropolarimeter (SOLARSPEL), together with MW images from the Siberian Radioheliograph (SRH). The flare was also observed by two imaging X-ray telescopes, Solar Orbiter/STIX and ASO-S/HXI. Nonlinear force-free field extrapolations are used to reconstruct the three-dimensional magnetic configuration of the AR. We present evidence for a direct coupling between the thermal plasma and the non-thermal electron population in the frame of collisionless plasma during the initial flare stage. Some simple relationships about electron acceleration process are presented and discussed. Analysis of the extrapolated magnetic field indicates that the flare onset was associated with a system of low-lying sheared magnetic loops located along the polarity inversion line (PIL). Given the confined nature of the event and the reconstructed magnetic configuration, we infer that magnetic reconnection most likely occurred within current sheets possessing a substantial guide-field component. The observed non-stationary QPPs in the non-thermal emission, with periods decreasing from approximately 15 to 9 s, are interpreted as signatures of a sequence of magnetic reconnection episodes occurring in different magnetic structures and triggered quasi-periodically by a process that remains uncertain, but which may involve propagating slow magnetoacoustic waves.
