The standard flare model, in 2D or 3D, considers a magnetic field configuration beneath the presence of a flux rope, the progenitor of a coronal mass ejection (CME). Although this has had much success in producing typical flare signatures, such as ribbons, it may not represent the complete picture. This is because flares can occur in regions without CMEs. We present magnetohydrodynamic (MHD) models that can simulate the large-scale effects of flares in CME and non-CME regions. By considering instabilities in the magnetic field and the subsequent reconnection and dynamic reorganization of the field, we can get a better understanding of the effects of impulsive flares. Investigating energy fluxes (both flows and Poynting transport) within the flaring volume and, in particular, how they relate spatially to the reconnected field, will give us a deeper insight into how the flare process transports energy from the coronal volume into the sharply defined features that we observe.