Quantitative Comparisons between WSA Implementations

• Published in: The Astrophysical journal Vol. 970; no. 1; pp. 35 - 43
• Main Authors: Jones, Shaela I., Caplan, Ronald M., Arge, C. Nick, Linker, Jon A., Henney, Carl J., Attie, Raphael, Downs, Cooper, Jha, Bibhuti Kumar, Turtle, James, Upton, Lisa
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.07.2024; IOP Publishing
• Subjects: Boundaries; Coronal magnetic fields; Finite difference method; Heliosphere; Interplanetary magnetic fields; Magnetic fields; Mathematical analysis; Model selection; Polar environments; Polar regions; Potential fields; Solar corona; Solar coronal lines; Solar magnetic field; Solar wind; Solar wind speed; Space weather; Spherical harmonics; Wind speed
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad50c9

Abstract The Wang–Sheeley–Arge (WSA) model has been in use for decades and remains a popular, economical approach to modeling the solar coronal magnetic field and forecasting conditions in the inner heliosphere. Given its usefulness, it is unsurprising that a number of WSA implementations have been developed by various groups with different computational approaches. While the WSA magnetic field model has traditionally been calculated using a spherical harmonic expansion of the solar magnetic field, finite-difference potential field solutions can offer speed and/or accuracy advantages. However, the creation of new versions of WSA requires that we ensure the solutions from these new models are consistent with established versions and that we quantify for the user community to what degree and in what ways they differ. In this paper, we present side-by-side comparisons of WSA models produced using the traditional, spherical harmonic–based implementation developed by Wang, Sheeley, and Arge with WSA models produced using a recently open-sourced finite-difference code from the CORHEL modeling suite called POT3D. We present comparisons of the terminal solar wind speed and magnetic field at the outer boundaries of the models, weighing these against the variation of the WSA model in the presence of small perturbations in the computational procedure, parameters, and inputs. We also compare the footpoints of magnetic field lines traced from the outer boundaries and the locations of open field in the models. We find that the traced field-line footpoints show remarkable agreement, with the greatest differences near the magnetic neutral line and in the polar regions.