Abstract <p>This study investigates the role of electromagnetic wave dynamics in heating the lower corona and upper chromosphere in M-type stars, which possess a non-relativistic, weakly magnetized, and partially degenerate electron-ion plasma environment. Kinetic modeling is used to investigate the behavior of low-frequency (Alfvén) and high-frequency (R and L) waves. The results demonstrate that R and L waves are found to transfer energy more effectively to the active magnetic corona, in contrast to Alfvén waves, which are primarily limited to the upper chromospheric region where they can deposit energy locally. Additionally, the effect of ion cyclotron frequency and propagation length on wave energy transfer and coronal heating in M stars is studied, which may be facilitated by a wave-dependent energy redistribution mechanism. Although this model assumes a completely ionized plasma that fits the upper chromosphere and corona, the impact of partial ionization in deeper layers could be important and needs further study. This study lays the foundation for understanding M-star magnetic activity and encourages future research that incorporates more complex plasma conditions.</p> Graphical abstract <p>. </p>