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In this work we describe our implementation of a thermodynamic energyequation into the global corona model of the Space Weather Modeling Framework(SWMF), and its development into the new Lower Corona (LC) model. This workincludes the integration of the additional energy transport terms of coronalheating, electron heat conduction, and optically thin radiative cooling intothe governing magnetohydrodynamic (MHD) energy equation. We examine twodifferent boundary conditions using this model; one set in the upper transitionregion (the Radiative Energy Balance model), as well as a uniform chromosphericcondition where the transition region can be modeled in its entirety. Viaobservation synthesis from model results and the subsequent comparison to fullsun extreme ultraviolet (EUV) and soft X-Ray observations of CarringtonRotation (CR) 1913 centered on Aug 27, 1996, we demonstrate the need for theseadditional considerations when using global MHD models to describe the uniqueconditions in the low corona. Through multiple simulations we examine abilityof the LC model to asses and discriminate between coronal heating models, andfind that a relative simple empirical heating model is adequate in reproducingstructures observed in the low corona. We show that the interplay betweencoronal heating and electron heat conduction provides significant feedback ontothe 3D magnetic topology in the low corona as compared to a potential fieldextrapolation, and that this feedback is largely dependent on the amount ofmechanical energy introduced into the corona.

Towards a Realistic, Data-Driven Thermodynamic MHD Model of the Global Solar Corona