外展环中反射衰减慢模波的数值模拟
Modelling of Reflective Propagating Slow-mode Wave in a Flaring Loop
摘要：
准周期性传播强度扰动已经在十多年的EUV图像中在大日冕环中观察到，并且被广泛接受为慢磁声波。然而，日出/EIS的光谱观测显示它们与持续的日冕上升流有关，这一解释值得商榷。我们进行了一个2.5维磁流体动力学模拟来模拟色球蒸发和耀斑环中的反射模式。我们的模型包括日冕，过渡区，色球层。我们证明了由合成的\textit{Solar Dynamics Observatory} /大气成像组件（AIA）131，94~ π发射图像捕获的准周期传播强度变化与以前的观测结果很好地匹配。用粒子示踪剂进行模拟，证实了这些准周期性的传播强度变化是由反射慢模波和质量流组成的，在一个平均温度为9 MK、长度为80 Mm的环中，质量流的平均速率为310 km/s。利用合成的\textit{Solar and Heliospheric Observatory} /太阳紫外辐射测量（SUMER）Fe XIX线发射的多普勒频移速度图和强度图，我们确认这些反射慢模波是传播波。
英文摘要：
Quasi-periodic propagating intensity disturbances have been observed in large coronal loops in EUV images over a decade, and are widely accepted to be slow magnetosonic waves. However, spectroscopic observations from Hinode/EIS revealed their association with persistent coronal upflows, making this interpretation debatable. We perform a 2.5D magnetohydrodynamic simulation to imitate the chromospheric evaporation and the following reflected patterns in a flare loop. Our model encompasses the corona, transition region, and chromosphere. We demonstrate that the quasi periodic propagating intensity variations captured by the synthesized \textit{Solar Dynamics Observatory}/Atmospheric Imaging Assembly (AIA) 131, 94~Å~emission images match the previous observations well. With particle tracers in the simulation, we confirm that these quasi periodic propagating intensity variations consist of reflected slow mode waves and mass flows with an average speed of 310 km/s in an 80 Mm length loop with an average temperature of 9 MK. With the synthesized Doppler shift velocity and intensity maps of the \textit{Solar and Heliospheric Observatory}/Solar Ultraviolet Measurement of Emitted Radiation (SUMER) Fe XIX line emission, we confirm that these reflected slow mode waves are propagating waves.
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