In this paper, we report the observed temporal correlation between extreme-ultraviolet (EUV) emission and magneto-acoustic oscillations in an EUV moss region, which is the footpoint region only connected by magnetic loops with million-degree plasma. The result is obtained from a detailed multi-wavelength data analysis of the region with the purpose of resolving fine-scale mass and energy flows that come from the photosphere, pass through the chromosphere and finally heat the solar transition region or the corona. The data set covers three atmospheric levels on the Sun, consisting of high-resolution broad-band imaging at TiO 7057 and the line of sight magnetograms for the photosphere, high-resolution narrow-band images at helium i 10830 for the chromosphere and EUV images at 171 for the corona. The 10830 narrow-band images and the TiO 7057 broad-band images are from a much earlier observation on 2012 July 22 with the 1.6 meter aperture Goode Solar Telescope (GST) at Big Bear Solar Observatory (BBSO) and the EUV 171 images and the magnetograms are from observations made by Atmospheric Imaging Assembly (AIA) or Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory (SDO). We report the following new phenomena: (1) Repeated injections of chromospheric material appearing as 10830 absorption are squirted out from inter-granular lanes with a period of ∼ 5 minutes. (2) EUV emissions are found to be periodically modulated with similar periods of ∼ 5 minutes. (3) Around the injection area where 10830 absorption is enhanced, both EUV emissions and strength of the magnetic field are remarkably stronger. (4) The peaks on the time profile of the EUV emissions are found to be in sync with oscillatory peaks of the stronger magnetic field in the region. These findings may give a series of strong evidences supporting the scenario that coronal heating is powered by magneto-acoustic waves.

在本文中，我们报告了在极紫外 (EUV) 苔藓区域中观察到的极紫外 (EUV) 发射和磁声振荡之间的时间相关性，该区域是仅由磁环与百万度等离子体连接的脚点区域。该结果来自对该区域的详细多波长数据分析，目的是解析来自光球层、穿过色球层并最终加热太阳过渡区域或日冕的精细质量和能量流。该数据集涵盖了太阳上的三个大气层，包括 TiO 7057 的高分辨率宽带成像和光球层的视线磁图，氦i的高分辨率窄带图像10830 用于色球层和 EUV 图像，171 用于日冕。10830 窄带图像和 TiO 7057 宽带图像来自 2012 年 7 月 22 日在大熊太阳天文台 (BBSO) 使用 1.6 米孔径古德太阳望远镜 (GST) 和 EUV 171 图像和磁力图来自太阳动力学天文台 (SDO) 上的大气成像组件 (AIA) 或日震和磁成像仪 (HMI) 的观测结果。我们报告了以下新现象：（1）重复注入表现为 10830 吸收的色球物质从粒间通道喷出，周期约为 5 分钟。(2) 发现 EUV 发射以 ∼ 5 分钟的类似周期进行周期性调制。(3) 10830吸收增强的注入区周围，EUV 发射和磁场强度都显着增强。(4) EUV 发射时间曲线上的峰值与该区域强磁场的振荡峰值同步。这些发现可能会提供一系列强有力的证据来支持日冕加热是由磁声波驱动的情景。