Diagnostic capabilities of spectropolarimetric observations for understanding solar phenomena

Future ground-based telescopes will expand our capabilities for simultaneous multi-line polarimetric observations in a wide range of wavelengths, from the near-ultraviolet to the near-infrared. This creates a strong demand to compare candidate spectral lines to establish a guideline of the lines tha...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2021-08, Vol.652
Main Authors: C. Quintero Noda, Barklem, P S, Gafeira, R, B. Ruiz Cobo, Collados, M, Carlsson, M, V. Martínez Pillet, D. Orozco Suárez, Uitenbroek, H, Katsukawa, Y
Format: Article
Language:English
Subjects:
Circular polarization
Hydrogen atoms
Inversions
Line spectra
Lower atmosphere
Magnetic properties
Parameter sensitivity
Photosphere
Response functions
Solar phenomena
Space telescopes
Spatial distribution
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Summary:Future ground-based telescopes will expand our capabilities for simultaneous multi-line polarimetric observations in a wide range of wavelengths, from the near-ultraviolet to the near-infrared. This creates a strong demand to compare candidate spectral lines to establish a guideline of the lines that are most appropriate for each observation target. We focused in this first work on Zeeman-sensitive photospheric lines in the visible and infrared. We first examined their polarisation signals and response functions using a 1D semi-empirical atmosphere. Then we studied the spatial distribution of the line core intensity and linear and circular polarisation signals using a realistic 3D numerical simulation. We ran inversions of synthetic profiles, and we compared the heights at which we obtain a high correlation between the input and the inferred atmosphere. We also used this opportunity to revisit the atomic information we have on these lines and computed the broadening cross-sections due to collisions with neutral hydrogen atoms for all the studied spectral lines. The results reveal that four spectral lines stand out from the rest for quiet-Sun and network conditions: Fe I 5250.2, 6302, 8468, and 15 648 Å. The first three form higher in the atmosphere, and the last line is mainly sensitive to the atmospheric parameters at the bottom of the photosphere. However, as they reach different heights, we strongly recommend using at least one of the first three candidates together with the Fe I 15 648 Å line to optimise our capabilities for inferring the thermal and magnetic properties of the lower atmosphere.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/202037735