  Magnetohydrodynamic waves are believed to play a significant role in coronal
heating, and could be used for remote diagnostics of solar plasma. Both the
heating and diagnostic applications rely on a correct inversion (or backward
modelling) of the observables into the thermal and magnetic structures of the
plasma. However, owing to the limited availability of observables, this is an
ill-posed issue. Forward Modelling is to establish a plausible mapping of
plasma structuring into observables. In this study, we set up forward models of
standing kink modes in coronal loops and simulate optically thin emissions in
the extreme ultraviolet bandpasses, and then adjust plasma parameters and
viewing angles to match three events of transverse loop oscillations observed
by the Solar Dynamics Observatory/Atmospheric Imaging Assembly. We demonstrate
that forward models could be effectively used to identify the oscillation
overtone and polarization, to reproduce the general profile of oscillation
amplitude and phase, and to predict multiple harmonic periodicities in the
associated emission intensity and loop width variation.
