AI 中文总结
研究利用太阳动力学天文台数据，首次成像检测到X1.6级耀斑中HFR足点漂移驱动的三维弧面-通量绳重联产生的特殊喷流，为标准耀斑模型的三维模拟扩展提供了新观测依据。
AI 中文摘要
利用太阳动力学天文台的多波段数据，我们首次成像检测到X1.6级太阳耀斑期间，由爆发热通道通量绳（HFR）的足点漂移驱动的重联喷流。结果表明，这些喷流是HFR爆发的固有副产物，与HFR足点漂移以及相关耀斑带钩的形态演化存在强时空耦合。与标准日冕喷流不同，这些喷流缺乏倒Y型形态，且与下方光球层的通量抵消或浮现无关联；它们表现为小尺度准直抛射物的集群，速度达180-200 km/s，兼具冷、热发射成分，在冷极紫外（EUV）通道（304埃和171埃）和热EUV通道（94埃）中均可观测到。成像观测显示，这些喷流由不断发生的三维弧面-通量绳（ar-rf）重联触发，触发机制是膨胀的HFR与周围日冕侧弧面的相互作用。观测到的喷流在形态和动力学上的复杂性表明，太阳爆发中正在进行的ar-rf重联具有间歇性和爆发性的本质。我们估算，驱动单个此类喷流需要局部磁场强度降低约9高斯。作为三维磁重联的直接特征，这些观测到的喷流明确了该过程的确切位置并表征了其性质，为标准耀斑模型的三维数值模拟扩展提供了新的观测视角。要充分了解这些喷流在太阳爆发中的普遍程度，还需对其开展更多观测案例研究。
英文摘要
Utilizing multi-wavelength data from the Solar Dynamics Observatory, we report the first imaging detection of reconnection jets driven by the footpoint drift of an erupting hot-channel flux rope (HFR) during an X1.6-class solar flare. Our results demonstrate that these jets are inherent byproducts of the HFR eruption, exhibiting strong spatiotemporal coupling with the HFR footpoint drift and the morphological evolution of the associated flare ribbon hooks. Unlike standard coronal jets, these ejections lack an inverted-Y morphology and show no association with underlying photospheric flux cancellation or emergence. They manifest as clusters of small-scale, collimated ejecta (180-200 km s$^{-1}$) featuring co-existing cool and hot emission components visible in both cool (304 and 171 Angstrom) and hot (94 Angstrom) EUV channels. The imaging observations reveal that these jets are triggered by successive 3D arcade-flux rope (ar-rf) reconnection as the expanding HFR interacts with the ambient coronal side arcades. The morphological and dynamic complexity of these observed jets implies that the ongoing ar-rf reconnection in solar eruptions is episodic and bursty in nature. Our estimates show that a decrease of approximately 9 G in localized magnetic field strength is required to power these individual jets. As direct signatures of 3D magnetic reconnection, these observed jets pinpoint the exact site and characterize the nature of the process, providing new observational insight into 3D numerical simulation extensions of the standard flare model. Further observational case studies of these jets are required to fully understand their prevalence across solar eruptions.
Comments12 pages, 5 figures, 3 animations; accepted for publication in The Astrophysical Journal Letters
