  Recent numerical studies of oscillating flux tubes have established the
significance of resonant absorption in the damping of propagating transverse
oscillations in coronal loops. The nonlinear nature of the mechanism has been
examined alongside the Kelvin-Helmholtz instability, which is expected to
manifest in the resonant layers at the edges of the flux tubes. While these two
processes have been hypothesized to heat coronal loops through the dissipation
of wave energy into smaller scales, the occurring mixing with the hotter
surroundings can potentially hide this effect. We aim to study the effects of
wave heating from driven and standing kink waves in a coronal loop. Using the
MPI-AMRVAC code, we perform ideal, three dimensional magnetohydrodynamic (MHD)
simulations of both (a) footpoint driven and (b) free standing oscillations in
a straight coronal flux tube, in the presence of numerical resistivity. We have
observed the development of Kelvin-Helmholtz eddies at the loop boundary layer
of all three models considered here, as well as an increase of the volume
averaged temperature inside the loop. The main heating mechanism in our setups
was Ohmic dissipation, as indicated by the higher values for the temperatures
and current densities located near the footpoints. The introduction of a
temperature gradient between the inner tube and the surrounding plasma,
suggests that the mixing of the two regions, in the case of hotter environment,
greatly increases the temperature of the tube at the site of the strongest
turbulence, beyond the contribution of the aforementioned wave heating
mechanism.
