Abstract　 　　
　 We investigate coronal energy flow during simulations of coronal mass ejections (CMEs). In these models, we place the CME in the context of the global corona using a numerical MHD code in spherical coordinates that includes a background solar wind. The equations we solve include coronal heating, thermal conduction and radiative cooling in the energy equation. In a 2.5D simulation, we examine the energy release in the current sheet as the eruption takes place, and find, as expected, that the Poynting flux is the dominant carrier of energy into the current sheet. The reconnection occurs low in the corona, so that the kinetic energy released from reconnection is greater in the sunward direction than the anti-sunward direction. There is also a significant flow of energy out of the sides of the current sheet into the upstream region due to thermal conduction along field lines and viscous drag. Expanding our simulations to three dimensions, we follow the physics responsible for plasma heating during the eruption, and find that the adiabatic compression plays an important role in heating plasma around the current sheet. For both of these simulations, we follow the formation and evolution of the current sheet and simulate emissions in the X-ray and extreme ultra-violet wavelengths in order to determine signatures of current sheet energetics in observations from the X-ray Telescope on the Hinode satellite and the AIA instrument on the Solar Dynamics Observatory.