Authors: Cooper Downs (PSI), Jon A. Linker (PSI), Peter Riley (PSI), Emily I. Mason (PSI), Ronald M. Caplan (PSI), Roberto Lionello (PSI)

In this poster we explore properties of a data-assimilative, data-driven, continuously evolving thermodynamic MHD simulation of the global solar corona. This simulation spans 32 days and 7 hours during the weeks leading up to and after the April 8th 2024 total solar eclipse. Because the simulation is driven by the continuous evolution of the surface flux distribution, which includes large-scale flux-emergence, helicity injection, supergranular flows, and random small-scale flux evolution, dynamical aspects emerge that cannot be captured in a traditional steady state MHD relaxation. Here we focus on how these dynamics pertain to our understanding of connectivity and plasma properties near structures that bound the open and closed corona. We map how open, closed, and disconnected fluxes evolve over time and relate to small-and large-scale topological features in the corona. We also explore how the temperatures and densities of the bounding plasma structures evolve in time. A comparison to several steady state calculations made over the same time period helps contrast the differences between these and the data-driven evolutionary calculation.