  High-frequency wave phenomena present a great deal of interest as one of the
possible candidates to contribute to the energy input required to heat the
corona as a part of the AC heating theory. However, the resolution of imaging
instruments up until the Solar Orbiter have made it impossible to resolve the
necessary time and spatial scales. The present paper reports on high-frequency
transverse motions in a small loop located in a quiet Sun region of the corona.
The oscillations were observed with the HRIEUV telescope (17.4 nm) of the EUI
instrument onboard the Solar Orbiter. We detect two transverse oscillations in
short loops with lengths of 4.5 Mm and 11 Mm. The shorter loop displays an
oscillation with a 14 s period and the longer a 30 s period. Despite the high
resolution, no definitive identification as propagating or standing waves is
possible. The velocity amplitudes are found to be equal to 72 km/s and 125
km/s, respectively, for the shorter and longer loop. Based on that, we also
estimated the values of the energy flux contained in the loops - the energy
flux of the 14 s oscillation is 1.9 kW m^-2 and of the 30 s oscillation it is
6.5 kW m^-2 . While these oscillations have been observed in the Quiet Sun,
their energy fluxes are of the same order as the energy input required to heat
the active solar corona. Numerical simulations were performed in order to
reproduce the observed oscillations. The correspondence of the numerical
results to the observations provide support to the energy content estimates for
the observations. Such high energy densities have not yet been observed in
decayless coronal waves, and this is promising for coronal heating models based
on wave damping.
