Testing, Comparing, and Validating an L1 Method for Abundances Derivations from EUV Spectra
4 affiliations
- 1SETI Institute
- 2Lockheed Martin Solar & Astrophysics Laboratory
- 3University of Oslo
- 4Harvard-Smithsonian Center for Astrophysics
Abstract
Element abundances found in the solar corona and solar wind are often different from those measured in the solar photosphere, and the fractionation mechanisms are thought to be intimately tied to the physical processes leading to coronal heating and acceleration of the solar wind. The complexity of the data and the methods used to invert underconstrained problems and thus estimate abundances make it challenging to identify and study these mechanisms. In this work, we present an L1-norm inversion method to derive abundances from coronal spectral observations. We explored a variety of approaches, considering different sets of inverted variables (e.g., including the abundance of Si, S, and Fe, as separate independent variables), and we tested and validated them using synthetic data from numerical radiative MHD models. In addition, we investigated the effects of bound-free absorption from neutral hydrogen and helium on the method and Poisson noise. We discuss the advantages and limitations of the various inversion approaches presented.
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BibTeX
@article{martinezsykora2026testing,
title = {{Testing, Comparing, and Validating an L1 Method for Abundances Derivations from EUV Spectra}},
author = {Juan Martínez-Sykora and Paola Testa and Viggo H. Hansteen},
journal = {The Astrophysical Journal},
year = {2026},
month = nov,
doi = {10.3847/1538-4357/aeb1a7},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeb1a7},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Testing, Comparing, and Validating an L1 Method for Abundances Derivations from EUV Spectra
AU - Juan Martínez-Sykora
AU - Paola Testa
AU - Viggo H. Hansteen
PY - 2026
DA - 2026/11/06
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/aeb1a7
UR - https://iopscience.iop.org/article/10.3847/1538-4357/aeb1a7
AB - Element abundances found in the solar corona and solar wind are often different from those measured in the solar photosphere, and the fractionation mechanisms are thought to be intimately tied to the physical processes leading to coronal heating and acceleration of the solar wind. The complexity of the data and the methods used to invert underconstrained problems and thus estimate abundances make it challenging to identify and study these mechanisms. In this work, we present an L1-norm inversion method to derive abundances from coronal spectral observations. We explored a variety of approaches, considering different sets of inverted variables (e.g., including the abundance of Si, S, and Fe, as separate independent variables), and we tested and validated them using synthetic data from numerical radiative MHD models. In addition, we investigated the effects of bound-free absorption from neutral hydrogen and helium on the method and Poisson noise. We discuss the advantages and limitations of the various inversion approaches presented.
SN - 1538-4357
SN - 0004-637X
ER -