Solar flares are driven by the release of magnetic energy and change in the topology of the underlying magnetic fields in a process called magnetic reconnection. Understanding that energy release and the subsequent evolution of the radiative and magnetohydrodynamic response of the plasma is vital to understanding magnetic reconnection, a fundamental process in astrophysical plasmas that occurs throughout the universe. Modern observations and modeling are required to make progress on this problem. The role of accelerated particles, magnetohydrodynamic waves, turbulence, and direct heating of the plasma will be examined. The goal of this work is to understand the interplay between the evolution of the magnetic field, the hydrodynamic response of the plasma, and the radiative output of flares. These processes will be investigated with a combination of simulations, observations, and forward modeling.