Magnetic tornadoes, characterized as impulsive Alfvén waves initiated by photospheric vortices in intergranular lanes, are considered efficient energy channels to the corona. Despite their acknowledged importance for solar coronal heating, their observational counterparts from the corona have not been well understood. To address this issue, we use a radiative magnetohydrodynamic simulation of a coronal loop with footpoints rooted in the upper convection zone and synthesize the chromospheric and coronal emissions corresponding to a magnetic tornado. Considering Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å and Solar Orbiter/Extreme Ultraviolet Imager 174 Å channels, our synthesis reveals that the coronal response to magnetic tornadoes can be observed as an EUV brightening of which the width is ∼2 Mm. This brightening is located above the synthesized chromospheric swirl observed in the Ca ii 8542 Å, Ca ii K, and Mg ii k lines, which can be detected by instruments such as the Swedish 1 m Solar Telescope/CRisp Imaging SpectroPolarimeter, Goode Solar Telescope/Fast Imaging Solar Spectrograph, and Interface Region Imaging Spectrograph. Considering the height correspondence of the synthesized brightening, magnetic tornadoes can be a mechanism for the small-scale EUV brightenings such as the solar “campfires.” Our findings indicate that coordinated observations encompassing the chromosphere to the corona are indispensable for comprehending the origin of coronal EUV brightenings.

中文翻译：

---

磁龙卷的综合合成：色球层漩涡的空间入射和极紫外增亮


磁龙卷风的特征是由粒间通道中的光球涡旋引发的脉冲阿尔文波，被认为是通往日冕的有效能量通道。尽管它们对太阳日冕加热的重要性已得到公认，但它们在日冕中的观测对应物尚未得到很好的了解。为了解决这个问题，我们使用日冕环的辐射磁流体动力学模拟，其足点植根于上对流区，并合成与磁龙卷风相对应的色球和日冕发射。考虑到太阳动力学天文台/大气成像组件 171 Å 和太阳轨道飞行器/极紫外成像仪 174 Å 通道，我们的综合表明，日冕对磁龙卷风的响应可以观察到宽度为 ∼2 Mm 的 EUV 增亮。这种增亮位于在 Ca 中观察到的合成色球漩涡上方二、 8542 埃, 钙二、钾和镁二、 k线，可以通过瑞典1 m太阳望远镜/CRisp成像分光偏振计、古德太阳望远镜/快速成像太阳摄谱仪、界面区域成像摄谱仪等仪器进行探测。考虑到合成增亮的高度对应性，磁龙卷风可以成为小规模 EUV 增亮的机制，例如太阳“篝火”。我们的研究结果表明，从色球层到日冕的协调观测对于理解日冕 EUV 增亮的起源是必不可少的。