Authors: Wraback, E. M. (University of Michigan), Landi, E. (University of Michigan), Manchester, W.B. (University of Michigan), Szente, J. (Boston University)

The charge states evolution of plasmas leaving the Sun freezes in low in the solar corona and carries information about the inner corona through the heliosphere, which in situ measurements can extract to study early solar wind and coronal mass ejection (CME) evolution and energetics. 3D global magnetohydrodynamics models allow us to link the measured in-situ charge states to the energetics in the inner corona, where many processes driving the evolution occur. This work uses the Alfvén Wave Solar atmosphere Model (AWSoM) to simulate the April 9^th, 2008, CME. We study the energy budget evolution in the CME as the non-equilibrium charge states freeze-in to understand what drives the plasmas’ evolution through the solar corona. Early in the eruption, a significant portion of the magnetic energy stored in the flux rope dissipates to the thermal or is converted to kinetic energy. The protons are preferentially heated by the compression in the CME sheath, increasing the Alfvén wave energy dissipation. At the backside and along the flanks of the CME, heating is by reconnection with the overlying pseudostreamer and nearby helmet streamer and coronal hole, increasing the ionization states of the charge states in localized regions.