Deciphering the Formation and Dynamics of Double-decker Filaments through Component Magnetic Reconnection

Dongxu Liu, Yuandeng Shen, Yi Bi, Zehao Tang, Chengrui Zhou and Surui Yao
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Abstract

The formation of double-decker filaments has long been an enigma in the field of solar physics. Using stereoscopic observations from the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory, we show that the double-decker filament formed on 2013 August 30 resulted from the splitting of a braided magnetic flux rope. The splitting was driven by component magnetic reconnection between intertwined field lines, triggered by the rotational motion in a part of one filament footpoint. This mechanism, inferred from observed small jets, brightenings, and bidirectional mass flows, differs from the previous conclusion attributing filament splitting to magnetic reconnection between the legs of confining magnetic field lines within or above the filament. The splitting speed might be modulated by the reconnection speed, as evidenced by the correspondence between the filament’s slow and fast rising phases and the intermittent and violent brightening stages. Following the splitting, the upper branch of the double-decker filament erupted as a coronal mass ejection, giving rise to a GOES soft X-ray M1.2 flare. In conclusion, our observations present a new formation mechanism for double-decker filaments, and the subsequent partial eruption is likely attributable to the torus instability of the background coronal magnetic field. Moreover, the detection of small jets within the filament provides new insights into the role of component magnetic reconnection in localized coronal heating processes.
通过分量磁重联解读双层细丝的形成和动力学
双层细丝的形成长期以来一直是太阳物理学领域的一个谜。利用太阳动力学观测站和日地关系观测站的立体观测,我们发现2013年8月30日形成的双层细丝是由编织的磁通绳断裂造成的。分裂是由缠绕在一起的磁场线之间的分量磁重联驱动的,由一个灯丝脚点部分的旋转运动触发。这一机制是从观测到的小喷流、变亮和双向质量流中推断出来的,它不同于先前的结论,即灯丝分裂是由于灯丝内部或上方的限制性磁场线腿之间的磁重联造成的。分裂速度可能受重连速度的调节,这可以从灯丝的缓慢和快速上升阶段与间歇和剧烈增亮阶段的对应关系中得到证明。在分裂之后,双层灯丝的上层分支以日冕物质抛射的形式爆发,产生GOES软x射线M1.2耀斑。综上所述,我们的观测提供了一种新的双层细丝形成机制,随后的部分喷发可能归因于背景日冕磁场的环面不稳定。此外,对细丝内小射流的检测为局部日冕加热过程中组件磁重联的作用提供了新的见解。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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