论文标题
HXR从激活的通量绳和随后的爆发长持续时间太阳耀斑的演变发射
HXR emission from an activated flux rope and subsequent evolution of an eruptive long duration solar flare
论文作者
论文摘要
在本文中，我们介绍了对主要M6.6长期事件（LDE）的进化阶段的全面研究，并特别强调了其爆发前阶段。该事件发生在2015年6月22日的NOAA 12371中。该事件的一个显着方面是一个持续大约一个小时的活跃前射击阶段，在此期间，热的EUV冠状通道处于堆积阶段，并显示了共同空间硬性X射线（HXR）发射至25 KEV的能量。因此，这是HXR冠状通道的第一个证据。基于NLFFF建模的冠状磁场构型清楚地表现出沿极性反转线（PIL）定向的磁通绳（MFR），并与冠状通道共同空间。我们观察到在$ \ $ \ $ 42小时的长期旋转形式，沿PIL的旋转形式，移动磁性特征和磁通取消的形式，我们观察到AR的光磁场发生了重大变化。在发作发作之前，MFR进行了缓慢上升阶段（$ \ $ \ $ 14 km s $^{ - 1} $）的$ \ $ \ $ \ $ 12分钟，我们将其归因于MFR本身的多个位置发生的链球切割重新连接的更快地堆积和激活MFR。 The sudden transition in the kinematic evolution of the MFR from the phase of slow to fast rise ($\approx$109 km s$^{-1}$ with acceleration $\approx$110 m s$^{-2}$) precisely divides the pre-flare and impulsive phase of the flare, which points toward the feedback process between the early dynamics of the eruption and the strength of the flare magnetic reconnection.
In this paper, we present a comprehensive study of the evolutionary phases of a major M6.6 long duration event (LDE) with special emphasize on its pre-flare phase. The event occurred in NOAA 12371 on 2015 June 22. A remarkable aspect of the event was an active pre-flare phase lasting for about an hour during which a hot EUV coronal channel was in build-up stage and displayed co-spatial hard X-ray (HXR) emission up to energies of 25 keV. As such, this is the first evidence of HXR coronal channel. The coronal magnetic field configuration based on NLFFF modeling clearly exhibited a magnetic flux rope (MFR) oriented along the polarity inversion line (PIL) and co-spatial with the coronal channel. We observed significant changes in the AR's photospheric magnetic field during an extended period of $\approx$42 hours in the form of rotation of sunspots, moving magnetic features, and flux cancellation along the PIL. Prior to the flare onset, the MFR underwent a slow rise phase ($\approx$14 km s$^{-1}$) for $\approx$12 min which we attribute to the faster build-up and activation of the MFR by tether-cutting reconnection occurring at multiple locations along the MFR itself. The sudden transition in the kinematic evolution of the MFR from the phase of slow to fast rise ($\approx$109 km s$^{-1}$ with acceleration $\approx$110 m s$^{-2}$) precisely divides the pre-flare and impulsive phase of the flare, which points toward the feedback process between the early dynamics of the eruption and the strength of the flare magnetic reconnection.
