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Diagnostic capabili...
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Noda, C. QuinteroUniv Oslo, Rosseland Ctr Solar Phys, POB 1029, N-0315 Oslo, Norway.;Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.;Inst Astrofis Canarias, Tenerife 38200, Spain.;Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
(författare)
Diagnostic capabilities of spectropolarimetric observations for understanding solar phenomena : I. Zeeman-sensitive photospheric lines
- Artikel/kapitelEngelska2021
Förlag, utgivningsår, omfång ...
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2021-08-27
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EDP Sciences,2021
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LIBRIS-ID:oai:DiVA.org:uu-455864
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https://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-455864URI
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https://doi.org/10.1051/0004-6361/202037735DOI
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Språk:engelska
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Sammanfattning på:engelska
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Ämneskategori:ref swepub-contenttype
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Ämneskategori:art swepub-publicationtype
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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 angstrom. 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 angstrom line to optimise our capabilities for inferring the thermal and magnetic properties of the lower atmosphere.
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Barklem, PaulUppsala universitet,Teoretisk astrofysik(Swepub:uu)pba11670
(författare)
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Gafeira, R.Inst Astrofis Andalucia CSIC, Apartado Correos 3004, Granada 18080, Spain.;Univ Coimbra, OGAUC, IA, DF, Coimbra, Portugal.
(författare)
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Ruiz Cobo, B.Inst Astrofis Canarias, Tenerife 38200, Spain.;Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
(författare)
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Collados, M.Inst Astrofis Canarias, Tenerife 38200, Spain.;Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.
(författare)
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Carlsson, M.Univ Oslo, Rosseland Ctr Solar Phys, POB 1029, N-0315 Oslo, Norway.;Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.
(författare)
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Pillet, V. MartinezUniv Colorado, Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA.
(författare)
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Orozco Suarez, D.Inst Astrofis Andalucia CSIC, Apartado Correos 3004, Granada 18080, Spain.
(författare)
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Uitenbroek, H.Univ Colorado, Natl Solar Observ, 3665 Discovery Dr, Boulder, CO 80303 USA.
(författare)
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Katsukawa, Y.Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan.
(författare)
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Univ Oslo, Rosseland Ctr Solar Phys, POB 1029, N-0315 Oslo, Norway.;Univ Oslo, Inst Theoret Astrophys, POB 1029, N-0315 Oslo, Norway.;Inst Astrofis Canarias, Tenerife 38200, Spain.;Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain.Teoretisk astrofysik
(creator_code:org_t)
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Ingår i:Astronomy and Astrophysics: EDP Sciences6520004-63611432-0746
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Noda, C. Quinter ...
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Barklem, Paul
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Gafeira, R.
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Ruiz Cobo, B.
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Collados, M.
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Carlsson, M.
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visa fler...
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Pillet, V. Marti ...
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Orozco Suarez, D ...
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Uitenbroek, H.
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Katsukawa, Y.
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