<p>We study the mechanisms of energy transfer and coronal formation in the accretion disks of neutron star (NS) remnants from neutron star-neutron star (NS-NS) collisions. Using magnetohydrodynamic (MHD) simulations with relativistic corrections to plasma inertia and quantum electrodynamics (QED) corrections to magnetic energy, we investigate the interplay of magnetic pressure, plasma pressure, and high-frequency Alfvén waves in the energy transit from the relativistic chromosphere to the non-relativistic corona. It shows that kinetic energy becomes important in the corona, preserving its dynamic structure and high temperatures, even though magnetic energy predominates in the chromosphere and is amplified by vacuum-polarization effects, driving energy transfer through Alfvén waves. Efficient energy redistribution is made possible in the transition region through wave-particle interactions and energy loss. These results improve our understanding of the dynamics of accretion disks in NS remnants and their function in the maintenance of high-energy astrophysical phenomena.</p>