基于NVST Hα观测的日珥羽流统计研究
Statistical Study of Solar Prominence Plumes Based on NVST H$α$ Observations
AI总结：
该研究基于NVST Hα观测数据，通过自动化图像处理流程统计34个日珥羽流，明确其参数特征与相关性，揭示羽流演化和触发机制的多样性，建立了日珥羽流统计框架。
AI中文摘要：
羽流是日珥中最具代表性的动力学特征之一，在日珥内部的物质与磁输运中发挥关键作用，但其物理本质和触发过程仍存在广泛争议。基于2013年至2025年间新真空太阳望远镜（New Vacuum Solar Telescope, NVST）的 limb Hα观测数据，我们开发了一套自动化图像处理流程，对34个演化清晰完整的羽流开展了统计研究。研究结果显示：羽流的寿命主要分布在300秒至700秒之间，垂直位移介于3至7兆米（Mm），平均宽度集中在0.5至1.5兆米，平均速度则处于10至20千米每秒（km s⁻¹）的范围。除分布范围较广外，羽流参数还呈现不规则的演化波动，表明不同羽流的形成与演化可能对应不同的物理模式。参数间的相关性分析进一步揭示：（1）寿命、垂直位移与平均宽度之间存在正相关关系，说明羽流的时间尺度与空间尺度存在内在耦合；（2）轨迹曲率与寿命、垂直位移、速度呈负相关，加速且宽度收缩的羽流通常曲率更低，提示曲率可能反映了环境影响及羽流的稳定性；（3）初始速度较高的羽流更易伴随前驱增亮现象，表明这类羽流可能由磁重联触发。此外，我们推断非泡状区域的部分羽流可能由微型暗条爆发驱动。这些结果为日珥羽流建立了统计框架，并揭示了其动力学演化与触发机制的多样性。
英文摘要：
Plumes are one of the most representative dynamic features observed in prominences and play a key role in mass and magnetic transport within them. However, their physical nature and triggering processes remain actively debated. Based on limb H$α$ observations from the New Vacuum Solar Telescope (NVST) during 2013--2025, we statistically investigated 34 plumes with clear and complete evolutions by developing an automated image-processing pipeline. It is revealed that plume lifetimes mainly range from 300 s to 700 s, with vertical displacements between 3--7 Mm. The mean widths and velocities are concentrated in the range of 0.5--1.5 Mm and 10--20 km s$^{-1}$, respectively. Besides wide distribution ranges, plume parameters exhibit irregular evolution fluctuations, indicating that the formation and evolution of various plumes may exhibit different physical patterns. Correlation analysis among the parameters further reveals that: (1) Positive correlations were found among lifetime, vertical displacement, and mean width, indicating an intrinsic coupling between the temporal and spatial scales of plumes. (2) Trajectory curvature is negatively correlated with lifetime, vertical displacement, and velocity. Accelerating and width-contracting plumes typically have lower curvature, suggesting that curvature may reflect environmental influences and the stability of plumes. (3) Plumes with higher initial velocities were more likely to be accompanied by precursor brightening, suggesting that these plumes may be triggered by magnetic reconnection. Furthermore, we infer that some plumes in non-bubble regions may be inherently driven by mini-filament eruptions. These results establish a statistical framework for prominence plumes and reveal diversity in their dynamical evolution and triggering mechanisms.
