  In this paper, we report the observed temporal correlation between
extreme-violet (EUV) emission and magneto-acoustic oscillations in a 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 to 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 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 \AA\ and the line of sight magnetograms for the photosphere,
high-resolution narrow-band images at Helium \textsc{i} 10830 \AA\ for the
chromosphere and EUV images at 171 \AA\ for the corona. We report following new
phenomena: 1) Repeated injections of chromospheric material shown as 10830 \AA\
absorption are squirted out from inter-granular lanes with the period of $\sim$
5 minutes. 2) EUV emissions are found to be periodically modulated with the
similar periods of $\sim$ 5 minutes. 3) Around the injection area where 10830
\AA\ absorption is enhanced, both EUV emissions and the strength of 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.
