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On 2019 July 2 a total solar eclipse -- visible across some parts of theSouthern Pacific Ocean, Chile and Argentina -- will enable observations of theSun's large-scale coronal structure. The structure of the Sun's corona andtheir emission characteristics are determined by underlying magnetic fieldswhich also govern coronal heating and solar eruptive events. However, coronalmagnetic field measurements remain an outstanding challenge. Computationalmodels of coronal magnetic fields serve an important purpose in this context.Earlier work has demonstrated that the large-scale coronal field is governed byslow surface flux evolution and memory build-up which allows for prediction ofthe coronal structure on solar rotational timescales. Utilizing this idea andbased upon a 51 day forward run of a data-driven solar surface flux transportmodel and a Potential Field Source Surface model, we predict the Sun's coronalstructure for the 2019 July 2 solar eclipse. We also forward model thepolarization characteristics of the coronal emission from the predictedmagnetic fields. We predict two large-scale streamer structures and theirlocations on the east and west limbs of the Sun and discuss the possibility ofdevelopment of a pseudo-streamer based on an analysis of field line topology.This study is relevant for coronal magnetometry initiatives from ground-basedfacilities such as the Daniel K. Inouye Solar Telescope and CoronalMultichannel Polarimeter, and upcoming space-based instruments such as theSolar Ultraviolet Imaging Telescope and the Variable Emission Line Coronagraphonboard ISRO's Aditya-L1 space mission.

The 2019 July 2 Total Solar Eclipse: Prediction of the Coronal Magnetic Field Structure and Polarization Characteristics