| Issue |
A&A
Volume 689, September 2024
|
|
|---|---|---|
| Article Number | A341 | |
| Number of page(s) | 9 | |
| Section | The Sun and the Heliosphere | |
| DOI | https://doi.org/10.1051/0004-6361/202450743 | |
| Published online | 25 September 2024 | |
Magnetic field diagnostics of prominences with the Mg II k line 3D Stokes inversions versus traditional methods
1
Astronomical Institute of the Czech Academy of Sciences, Fričova 298, 25165 Ondřejov, Czech Republic
2
Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain
3
Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
4
Consejo Superior de Investigaciones Científicas, Spain
Received:
16
May
2024
Accepted:
30
July
2024
The Mg II k resonance line is commonly used for diagnosing the solar chromosphere. We theoretically investigated its intensity and polarization in solar prominences, taking 3D radiative transfer and Hanle and Zeeman effects into account. We used an optically thick 3D model representative of a solar prominence and applied several inversion methods to the synthetic Stokes profiles, clarifying their pros and cons for inferring prominence magnetic fields. We conclude that the self-consistent 3D inversion with radiative transfer is necessary to determine the magnetic field vector, although its geometry cannot be inferred with full fidelity. We also demonstrate that more traditional methods, such as those based on the weak field approximation or the constant-property slab assumption, can offer useful information under certain conditions.
Key words: polarization / radiative transfer / Sun: filaments / prominences / Sun: magnetic fields
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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