标题： 高速日冕物质抛射形成的太阳暗条爆发的统计研究 显示英文标题

标题： A Statistical Study of Solar Filament Eruptions That Forms High-Speed Coronal Mass Ejections

摘要： 日冕物质抛射（CME）在驱动空间天气方面起着决定性作用，特别是那些快速的CME（例如，速度超过$800$~km~s$^{-1}$的）。理解快速CME的触发机制可以帮助我们更好地预测它们。 伴随着CME发生的(filament)爆发提供了研究CME早期演化的良好示踪剂。在这里，我们调查了66个伴随(filament)爆发的快速CME，分析了触发机制（即磁重联或理想MHD过程）、相关的flare和CME速度之间的相关性。 基于从SDO、GONG和STEREO收集的数据，我们发现：(1) 活跃区（AR）(filament)爆发和中间(filenent)（IFs）爆发比宁静区（QS）(filament)爆发更有可能产生快速CME，而极冠（PC）(filament)爆发在我们的统计中概率为零；(2) 产生快速CME的AR (filament)爆发更可能由磁重联触发，而QS和IFs更可能由理想MHD过程触发；(3) 对于AR (filament)和IFs，特定的触发机制似乎对最终产生的CME速度没有显著影响，而对于QS (filament)，理想MHD机制更有可能生成更快的CME；(4) 与之前的统计研究相比，(filament)爆发的起始高度和上覆磁场的衰减指数显示出一些差异：对于AR (filament)和IFs，衰减指数较大且更接近理论阈值，而对于QS (filament)，起始高度高于之前得到的结果。 显示英文摘要

摘要： Coronal mass ejections (CMEs) play a decisive role in driving space weather, especially, the fast ones (e.g., with speeds above $800$~km~s$^{-1}$). Understanding the trigger mechanisms of fast CMEs can help us gaining important information in forecasting them. The filament eruptions accompanied with CMEs provide a good tracer in studying the early evolution of CMEs. Here we surveyed 66 filament-accompanied fast CMEs to analyse the correlation between the trigger mechanisms, namely either magnetic reconnection or ideal MHD process, associated flares, and CME speeds. Based on the data gathering from SDO, GONG and STEREO, we find that: (1) Active region (AR) filament and intermediate filaments (IFs) eruptions show a higher probability for producing fast CMEs than quiet Sun (QS) filaments, while the probability of polar crown (PC) filament eruptions is zero in our statistic; (2) AR filament eruptions that produce fast CMEs are more likely triggered by magnetic reconnection, while QS and IFs are more likely triggered by ideal MHD process; (3) For AR filaments and IFs, it seems that the specific trigger mechanism does not have a significant influence on the resulted CME speeds, while for the QS filaments, the ideal MHD mechanism can more likely generate a faster CME; (4) Comparing with previous statistic study, the onset heights of filament eruptions and the decay indexes of the overlying field show some differences: for AR filaments and IFs, the decay indexes are larger and much closer to the theoretical threshold, while for QS filaments, the onset heights are higher than those obtained in previous results.