  In recent years, a number of numerical studies have been focusing on the
significance of the Kelvin-Helmholtz instability (KHI) in the dynamics of
oscillating coronal loops. This process enhances the transfer of energy into
smaller scales, and has been connected with heating of coronal loops, when
dissipation mechanisms, such as resistivity, are considered. However, the
turbulent layer is expected near the outer regions of the loops. Therefore, the
effects of wave heating are expected to be confined to the loop's external
layers, leaving their denser inner parts without a heating mechanism. In the
current work we aim to study the spatial evolution of wave heating effects from
a footpoint driven standing kink wave in a coronal loop. Using the MPI-AMRVAC
code, we performed ideal, three dimensional magnetohydrodynamic simulations of
footpoint driven transverse oscillations of a cold, straight coronal flux tube,
embedded in a hotter environment. We have also constructed forward models for
our simulation using the FoMo code. The developed Transverse Wave Induced
Kelvin-Helmholtz (TWIKH) rolls expand throughout the tube cross-section, and
cover it entirely. This turbulence significantly alters the initial density
profile, leading to a fully deformed cross section. As a consequence, the
resistive and viscous heating rate both increase over the entire loop cross
section. The resistive heating rate takes its maximum values near the
footpoints, while the viscous heating rate at the apex. We conclude that even a
monoperiodic driver can spread wave heating over the whole loop cross section,
potentially providing a heating source in the inner loop region. Despite the
loop's fully deformed structure, forward modelling still shows the structure
appearing as a loop.
