  We present a study of multi-wavelength observations, of a C 2.3 solar flare
in Active Region NOAA 12353, observed on 2015 May 23, which reveal new
properties of acoustic waves in the flaring region. The space-, and
ground-based data measured by the HELioseismological Large Regions
Interferometric Device, operating at the Vacuum Tower Telescope, the
Atmospheric Imaging Assembly, and Helioseismic and Magnetic Imager on board the
Solar Dynamic Observatory, were used in this paper. First, using power spectra
of solar oscillations, we identified the dominant frequencies and their
location at seven different atmospheric levels before and after the flare
event. Second, based on AIA observations taken in six Extreme Ultraviolet
filters, we derived Differential Emission Measure (DEM) profiles and DEM maps
of the flare. Finally, we confirm the {\sigma}-classification of the magnetic
field in the active area, directly related to the flare. Our results are as
follows: the high-frequency waves ({\nu}>5 mHz) in the photosphere, in both
cases, before and after the flare, are generated at the foot-points of the
chromospheric loop, while in the chromosphere (H{\alpha} line), before the
event the power enhancement exhibits for maximum of flare emission, and after
the eruption the enhancement by all frequencies is observed only in the post
flare loop area. Moreover, the power of oscillation in the pores surrounding
area before the flare has a random character, while after the flare
oscillation's power is concentrated in the pore, and weakened outside of. We
conclude that the accurate detection of high-frequency acoustic waves in the
active regions can lead to faster and easier prediction of high-energy events.
