Inferring 3D Coronal Magnetic Fields through Seismology-assisted Inversions of IQU-only Spectropolarimetric Observations

arXiv:2607.12846 · astro-ph.SR · Submitted 2026-07-14 · Read on arXiv

astro-ph.SR

Submitted: 2026-07-14

Updated: 2026-08-25

Comments: 16 pages. Accepted for publication in The Astrophysical Journal

Code: https://github.com/arparaschiv/solar-coronal-inversion

License: http://creativecommons.org/licenses/by/4.0/

The gist: The routine measurements of the Stokes IQUV signals of emission lines in the solar corona is still a challenging endeavor, particularly for observations using small-aperture instruments.

Terminology

Abstract

The routine measurements of the Stokes IQUV signals of emission lines in the solar corona is still a challenging endeavor, particularly for observations using small-aperture instruments. Therefore, recent studies have explored the use of coronal seismology and propagating Alfv'enic waves as alternative diagnostics of the coronal magnetic field. In particular, Yang et al. (2024) showed that plane-of-sky (POS) phase-speed measurements provide a direct and consistent diagnostic of the POS magnetic-field component (B POS). Building on recent theoretical advances in solar coronal polarization, we devise a novel inversion scheme and extended the CLEDB software package (Paraschiv & Judge 2022) to exploit Stokes IQU observations of two coronal emission lines combined with coronal-seismology derived B POS estimations. Using this framework, we perform a comprehensive statistical analysis demonstrating that this combination of diagnostics allows us to infer both magnetic field orientation and strength with an accuracy comparable to that of Stokes IQUV spectropolarimetry. This type of diagnostics is particularly suited for the Fe XIII 1074.7 nm and 1079.8 nm line pair routinely observed by new-generation instruments such as DKIST Cryo-NIRSP, DL-NIRSP, MLSO CoMP/UCoMP, and targeted by the future COSMO and CORSAIR efforts.

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