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On 21 August 2017 a total solar eclipse swept across the contiguous UnitedStates providing excellent opportunities for diagnostics of the Sun's corona.The Sun's coronal structure is notoriously difficult to observe except duringsolar eclipses; thus theoretical models must be relied upon for inferring theunderlying magnetic structure of the Sun's outer atmosphere. These models arenecessary for understanding the role of magnetic fields in the heating of thecorona to a million degrees and generation of severe space weather. Here wepresent a methodology for predicting the structure of the coronal field basedon long-term surface flux transport simulations whose output is utilized toextrapolate the coronal magnetic field structures. This prescription wasapplied to the 21 August 2017 solar eclipse. Post-eclipse analysis shows goodagreement between model simulated and observed coronal structures and theirlocations on the limb. We demonstrate that slow changes in the Sun's surfacemagnetic field distribution driven by long-term flux emergence and evolutiongovern large-scale coronal structures with a (plausibly cycle-phase dependent)dynamical memory timescale on the order of few solar rotations -- opening upthe possibility of large-scale, global corona predictions at least a month inadvance.

Solar Surface Magnetic Field Simulation Enabled Prediction of the  Large-Scale Coronal Structure of the 21 August 2017 Great American Eclipse:  An Assessment of Model Predictions and Observations