Evolution of the sheared magnetic fields of two X class flares observed by Hinode XRT
Evolution of the sheared magnetic fields of two X class flares observed by Hinode XRT
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DOI：
10.1093/pasj/59.sp3.s785
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发表时间：
2007-11
影响因子：
2.3
通讯作者：
Yingna Su;L. Golub;A. A. Ballegooijen-A.;E. DeLuca;K. Reeves;T. Sakao;R. Kano;N. Narukage;K. Shibasaki
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文献类型：
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作者：
Yingna Su;L. Golub;A. A. Ballegooijen-A.;E. DeLuca;K. Reeves;T. Sakao;R. Kano;N. Narukage;K. Shibasaki
我们目前的剪切磁场的演变在NOAA活动区10930，其中两个X级耀斑发生在2006年12月13日和12月14日，分别多波长观测。利用日出号上的X射线望远镜（XRT）和太阳光学望远镜（SOT）进行的观测表明，在这个活跃区域逐渐形成的剪切磁场是由一个新兴太阳黑子的旋转和自西向东运动造成的。在两个耀斑的前耀斑阶段，XRT显示了核心场区域的几个高度剪切的X射线环，对应于TRACE EUV观测中看到的灯丝。XRT观测还显示，剪切核心场的一部分爆发，而剪切核心场的另一部分在耀斑期间留下，这可能解释了为什么在耀斑之后TRACE仍然看到大部分的暗条。每次耀斑达到峰值后约2 - 3小时，核心场在XRT中再次变得可见，并显示出高度剪切的内部结构和较少剪切的外部结构。我们还发现，耀斑后的核心领域是明显小于剪切比耀斑前的核心领域，这是一致的想法，在耀斑期间释放的能量存储在高度剪切领域之前的耀斑。
We present multi-wavelength observations of the evolution of the sheared magnetic fields in NOAA Active Region 10930, where two X-class flares occurred on 2006 December 13 and December 14, respectively. Observations made with the X-ray Telescope (XRT) and the Solar Optical Telescope (SOT) aboard Hinode suggest that the gradual formation of the sheared magnetic fields in this active region is caused by the rotation and west-to-east motion of an emerging sunspot. In the pre-flare phase of the two flares, XRT shows several highly sheared X-ray loops in the core field region, corresponding to a filament seen in the TRACE EUV observations. XRT observations also show that part of the sheared core field erupted, and another part of the sheared core field stayed behind during the flares, which may explain why a large part of the filament is still seen by TRACE after the flare. About 2 - 3 hours after the peak of each flare, the core field becomes visible in XRT again, and shows a highly sheared inner and less-sheared outer structure. We also find that the post-flare core field is clearly less sheared than the pre-flare core field, which is consistent with the idea that the energy released during the flares is stored in the highly sheared fields prior to the flare.