Sun’s outer atmosphere is a million degree hotter than it’s visible surface, which is not understood with any of the known laws of thermodynamics and remains an intriguing problem for the astrophysics in general. It is now believed that most of the energy dissipation phenomenon occurs at the interface region in between solar chromosphere and corona, which is a highly dynamic, gravitationally stratified, nonlinear, inhomogeneous environment. Observed dynamics of thin magnetic flux tube structures in this layer, reflects the confined magnetohydrodynamic (MHD) wave-modes (kink, sausage and torsional Alfv ́en). For the first time, the evolution of the resultant transverse displacement of the observed flux tube structures, estimated from perpendicular velocity components, is analyzed along with cross-sectional width, photometric and azimuthal shear/torsion variations, to accurately identify the confined wave-mode(s). In my talk, I will discuss the observational evidence of pulse-like nonlinear kink wave-mode(s), as indicated by the strong coupling in between kinematic observables, with a frequency-doubling, -tripling aspect, supported by mutual phase relations centered around 0◦ and ±180◦ (Sharma et al. 2018). The 3D ensemble of the observed dynamic components revealed complexities pertinent to the accurate identification and interpretation of e.g. linear/nonlinear, coupled/uncoupled MHD wave-modes in the observed waveguides (spicules).