The 8 April 2024 total solar eclipse (TSE) provides a unique opportunity to study the solar corona. This work presents our prediction of the solar corona at the time of the eclipse based on magnetohydrodynamic (MHD) modeling performed with the Alfv\'{e}n Wave Solar Model-Realtime (AWSoM-R) in the Space Weather Modeling Framework, developed at the University of Michigan. We performed multiple simulations made with data input in the form of synchronic magnetograms from four sources, i.e., ADAPT-GONG, Lockheed Martin ESFAM, HipFT and NSO-NRT magnetograms. Simulations also include a higher-resolution model and a post-eclipse model incorporating newly emerged active regions. Our study fundamentally focuses on the limitations imposed by the lack of global solar observations, particularly on how these limitations affect coronal simulations. Specifically, we examine how differences among the magnetograms and the absence of observations from the east limb, due to the Sun's rotation, impact the accuracy of the predicted coronal structures. We synthesized a variety of representative observables, including the white-light and extreme-ultraviolet images from each model, and compared them with observations. The synthesized observables show remarkable differences because of the distinct magnetic coronal topologies, which stem from the varied magnetic flux distributions and the gaps in observational coverage. Our findings emphasize the need for comprehensive and multi-satellite magnetic field observations to improve future solar corona predictions.
@article{arxiv.2503.10974,
title = {Forecasting the 8 April 2024 Total Solar Eclipse with Multiple Solar Photospheric Magnetograms},
author = {Xianyu Liu and Weihao Liu and Ward B. Manchester and Daniel T. Welling and Gábor Tóth and Tamas I. Gombosi and Marc L. DeRosa and Luca Bertello and Alexei A. Pevtsov and Alexander A. Pevtsov and Kevin Reardon and Kathryn Wilbanks and Amy Rewoldt and Lulu Zhao},
journal= {arXiv preprint arXiv:2503.10974},
year = {2025}
}