Center-to-limb variation of spectral lines and continua observed with SST/CRISP and SST/CHROMIS

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Pietrow, Alexander G. M.,1991-Stockholms universitet,Institutionen för astronomi,Leibniz-Institut für Astrophysik Potsdam (AIP), Germany (author)

Center-to-limb variation of spectral lines and continua observed with SST/CRISP and SST/CHROMIS

Article/chapterEnglish2023

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2023-03-17
EDP Sciences,2023
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LIBRIS-ID:oai:DiVA.org:su-216958
https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-216958URI
https://doi.org/10.1051/0004-6361/202244811DOI

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Language:English
Summary in:English

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Subject category:ref swepub-contenttype
Subject category:art swepub-publicationtype

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Context. Observations of center-to-limb variations (CLVs) of spectral lines and continua provide a good test for the accuracy of models with a solar and stellar atmospheric structure and spectral line formation. They are also widely used to constrain elemental abundances, and are becoming increasingly more important in atmospheric studies of exoplanets. However, only a few such data sets exist for chromospheric lines.Aims. We aim to create a set of standard profiles by means of mosaics made with the CRISP and CHROMIS instruments of the Swedish 1-m Solar Telescope (SST), as well as to explore the robustness of said profiles obtained using this method.Methods. For each spectral line, we used a mosaic that ranges from the center to the limb. Each of these mosaics were averaged down to 50 individual spectral profiles and spaced by 0.02 in the μ scale. These profiles were corrected for p-mode oscillations, and their line parameters (equivalent width, line shift, full-width at half-maximum, and line depth) were then compared against literature values whenever possible.Results. We present a set of 50 average profiles that are spaced equidistantly along the cosine of the heliocentric angle (μ) by steps of 0.02 for five continuum points between 4001 and 7772 Å, as well as ten of the most commonly observed spectral lines at the SST (Ca II H & K, Ηβ, Mg I 5173 Å, C I 5380 Å, Fe I 6173 Å, Fe I 6301 Å, Ha, O I 7772 Å, and Ca II 8542 Å).Conclusions. The CLV of line profiles and continua are shared in the CDS as machine readable tables, providing a quantitative constraint on theoretical models that aim to model stellar atmospheres.

Subject headings and genre

NATURVETENSKAP Fysik Astronomi, astrofysik och kosmologi hsv//swe
NATURAL SCIENCES Physical Sciences Astronomy, Astrophysics and Cosmology hsv//eng
methods: observational
line: formation
Sun: photosphere
Sun: chromosphere
Sun: atmosphere

Added entries (persons, corporate bodies, meetings, titles ...)

Kiselman, Dan,1963-Stockholms universitet,Institutionen för astronomi(Swepub:su)dan (author)
Andriienko, Oleksii,1972-Stockholms universitet,Institutionen för astronomi(Swepub:su)olad6860 (author)
Petit Dit de la Roche, D. J. M. (author)
Díaz Baso, Carlos José,1991-Stockholms universitet,Institutionen för astronomi,University of Oslo, Norway(Swepub:su)cada4215 (author)
Calvo, Flavio,1988-Stockholms universitet,Institutionen för astronomi(Swepub:su)flca3632 (author)
Stockholms universitetInstitutionen för astronomi (creator_code:org_t)

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In:Astronomy and Astrophysics: EDP Sciences6710004-63611432-0746

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