论文标题

使用新的面膜拟合方法对冠状波面的三维重建

Three-Dimensional Reconstructions of Coronal Wave Surfaces Using a New Mask-Fitting Method

论文作者

Feng, Li, Lu, Lei, Inhester, Bernd, Plowman, Joseph, Ying, Beili, Mierla, Marilena, West, Matthew J., Gan, Weiqun

论文摘要

冠状波是通常由冠状质量弹出(CME)驱动的大规模干扰。我们研究了2012年3月7日的壮观波动事件,该事件与X5.4耀斑(Sol2012-03-07)有关。通过使用跑步的中心媒体(RCM)过滤方法来检测极端紫外线(EUV)图像中的时间变化,我们可以通过使用活跃的Pixel系统检测器和图像处理(在板上)(在板上)(shop project on Project in Boards Onboard)上板上(SDO)上的大气成像组装(AIA)观察到的EUV干扰(AIA)。在Coronagraph图像中,观察到Halo Front是EUV干扰的上部。基于从三个不同角度观察到的EUV和Coronagraph图像,我们使用新的掩码拟合方法对波面进行了三维(3D)重建。将重建与从前拟合方法获得的重建进行了比较。我们表明,掩模拟合方法可以通过捕获冲击波前线的凹形形状来反映不均匀的冠状介质。随后,我们追踪发展中的凹形结构并得出脱水的波浪运动学。 3D波鼻的​​速度从低于几百$ \ mathrm {km \,s^{ - 1}} $的低点增加到最大值约为3800 $ \ mathrm {km \,s^{ - 1}} $,然后慢慢减少。凹形结构开始更早减速,并且速度明显低于波鼻的速度。我们还发现,扩展的电晕中的3D波速度远高于整个太阳能磁盘的EUV干扰速度。

Coronal waves are large-scale disturbances often driven by coronal mass ejections (CMEs). We investigate a spectacular wave event on 7 March 2012, which is associated with an X5.4 flare (SOL2012-03-07). By using a running center-median (RCM) filtering method for the detection of temporal variations in extreme ultraviolet (EUV) images, we enhance the EUV disturbance observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) and the Sun Watcher using Active Pixel System detector and Image Processing (SWAP) onboard the PRoject for Onboard Autonomy 2 (PROBA2). In coronagraph images, a halo front is observed to be the upper counterpart of the EUV disturbance. Based on the EUV and coronagraph images observed from three different perspectives, we have made three-dimensional (3D) reconstructions of the wave surfaces using a new mask-fitting method. The reconstructions are compared with those obtained from forward-fitting methods. We show that the mask fitting method can reflect the inhomogeneous coronal medium by capturing the concave shape of the shock wave front. Subsequently, we trace the developing concave structure and derive the deprojected wave kinematics. The speed of the 3D-wave nose increases from a low value below a few hundred $\mathrm{km\,s^{-1}}$ to a maximum value of about 3800 $\mathrm{km\,s^{-1}}$, and then slowly decreases afterwards. The concave structure starts to decelerate earlier and has significantly lower speeds than those of the wave nose. We also find that the 3D-wave in the extended corona has a much higher speed than the speed of EUV disturbances across the solar disk.

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