The solar coronal heating dilemma, why the solar corona is orders of magnitude hotter than the solar photosphere, remains one of the central questions in space physics. Among the mechanisms proposed to explain the solar coronal heating phenomenon, energy transport and dissipation through MHD and kinetic-scale waves remains as the leading candidate. The focus of this session is to investigate the impacts of MHD and kinetic scale waves on the solar coronal heating, uniquely bringing together experts to discuss solar coronal heating via waves across MHD and kinetic regimes. We invite contributions from observational and simulation studies spanning MHD and kinetic regimes. The discussions in this session will improve our understanding of not only processes that contribute to solar coronal heating but also the comparison of the the macro-scale impacts to micro-scale impacts, providing new insights into the fundamentals of plasma dynamics in the solar and other astrophysical plasmas.