Recent observations of coronal loops reveal ubiquitous transverse
velocity perturbations, that undergo strong damping as they propagate.
Observational estimates show that these perturbations contain
significant amounts of energy. We have previously demonstrated that
this observed rapid damping can be understood in terms of coupling of
different wave modes in the inhomogeneous boundaries of the loops:
this mode coupling leads to the coupling of the transversal (kink)
mode to the azimuthal (Alfvén) mode, observed as the decay of the
transverse kink oscillations. However, an important point to note here
is that (observed) wave damping does not automatically imply
dissipation, and hence heating. To investigate under which
circumstances this process can contribute to the coronal heating and
to what extend the heating rate is sustainable, we perform 3D
numerical experiments modelling the observed, transverse oscillations
including the effects of resistivity, thermal conduction and radiative
losses. We take into considerations different amplitudes of the
driver, in a range from 2 km/s to 100 km/s, and model both
single-harmonic and broadband drivers. Forward modelling is used to
derive observable signatures.