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.

中文翻译：

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使用新的掩模拟合方法对日冕波表面进行三维重建

日冕波是大规模的扰动，通常由日冕物质抛射（CME）驱动。我们调查了 2012 年 3 月 7 日发生的与 X5.4 耀斑有关的壮观波浪事件 (SOL2012-03-07)。通过使用运行中心中值 (RCM) 过滤方法来检测极紫外 (EUV) 图像的时间变化，我们增强了太阳动力学天文台 (SDO) 上的大气成像组件 (AIA) 和Sun Watcher 使用主动像素系统检测器和图像处理 (SWAP) 板载 Autonomy 2 (PROBA2) 项目。在日冕图像中，可以观察到光晕前沿是 EUV 扰动的上部对应物。基于从三个不同角度观察到的 EUV 和日冕图像，我们使用新的掩模拟合方法对波面进行了三维 (3D) 重建。将重建与从前向拟合方法获得的重建进行比较。我们表明，面罩拟合方法可以通过捕获冲击波前的凹面形状来反射非均匀的日冕介质。随后，我们追踪发展中的凹面结构并推导出去投影的波运动学。3D 波鼻的速度从低于几百 $\mathrm{km\,s^{-1}}$ 的低值增加到大约 3800 $\mathrm{km\,s^{- 1}}$，然后缓慢下降。凹面结构开始减速较早，速度明显低于波头。