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Non-LTE line formation of Fe in late-type stars - IV. Modelling of the solar centre-to-limb variation in 3D
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Number of Authors: 10
2017 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 468, no 4, 4311-4322 p.Article in journal (Refereed) Published
Abstract [en]

Our ability to model the shapes and strengths of iron lines in the solar spectrum is a critical test of the accuracy of the solar iron abundance, which sets the absolute zero-point of all stellar metallicities. We use an extensive 463-level Fe atom with new photoionization cross-sections for Fe I and quantum mechanical calculations of collisional excitation and charge transfer with neutral hydrogen; the latter effectively remove a free parameter that has hampered all previous line formation studies of Fe in non-local thermodynamic equilibrium (NLTE). For the first time, we use realistic 3D NLTE calculations of Fe for a quantitative comparison to solar observations. We confront our theoretical line profiles with observations taken at different viewing angles across the solar disc with the Swedish 1-m Solar Telescope. We find that 3D modelling well reproduces the observed centre-to-limb behaviour of spectral lines overall, but highlight aspects that may require further work, especially cross-sections for inelastic collisions with electrons. Our inferred solar iron abundance is log(epsilon(Fe)) = 7.48 +/- 0.04 dex.

Place, publisher, year, edition, pages
2017. Vol. 468, no 4, 4311-4322 p.
Keyword [en]
atomic data, line: formation, methods: numerical, methods: observational, Sun: abundances, Sun: atmosphere
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-144759DOI: 10.1093/mnras/stx673ISI: 000402819700043OAI: oai:DiVA.org:su-144759DiVA: diva2:1127688
Available from: 2017-07-18 Created: 2017-07-18 Last updated: 2017-07-18Bibliographically approved

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Kiselman, DanLeenaarts, Jorrit
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