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Non-LTE line formation of Fe in late-type stars - III. 3D non-LTE analysis of metal-poor stars
Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia..
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy. Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany..
Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia..
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Observational Astronomy.
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2016 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 463, no 2, 1518-1533 p.Article in journal (Refereed) Published
Abstract [en]

As one of the most important elements in astronomy, iron abundance determinations need to be as accurate as possible. We investigate the accuracy of spectroscopic iron abundance analyses using archetypal metal-poor stars. We perform detailed 3D non-LTE radiative transfer calculations based on 3D hydrodynamic STAGGER model atmospheres, and employ a new model atom that includes new quantum-mechanical neutral hydrogen collisional rate coefficients. With the exception of the red giant HD122563, we find that the 3D non-LTE models achieve Fe I/Fe II excitation and ionization balance as well as not having any trends with equivalent width to within modelling uncertainties of 0.05 dex, all without having to invoke any microturbulent broadening; for HD122563 we predict that the current best parallax-based surface gravity is overestimated by 0.5 dex. Using a 3D non-LTE analysis, we infer iron abundances from the 3D model atmospheres that are roughly 0.1 dex higher than corresponding abundances from 1D MARCS model atmospheres; these differences go in the same direction as the non-LTE effects themselves. We make available grids of departure coefficients, equivalent widths and abundance corrections, calculated on 1D MARCS model atmospheres and horizontally and temporally averaged 3D STAGGER model atmospheres.

Place, publisher, year, edition, pages
2016. Vol. 463, no 2, 1518-1533 p.
Keyword [en]
line: formation, radiative transfer, methods: numerical, stars: abundances, stars: atmospheres
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-311177DOI: 10.1093/mnras/stw2077ISI: 000388122400031OAI: oai:DiVA.org:uu-311177DiVA: diva2:1059411
Funder
Australian Research Council, FL110100012Swedish Research Council, 2015-00415_3The Royal Swedish Academy of SciencesWenner-Gren FoundationsGöran Gustafsson Foundation for promotion of scientific research at Uppala University and Royal Institute of TechnologySwedish Research CouncilKnut and Alice Wallenberg FoundationDanish National Research Foundation, DNRF106
Available from: 2016-12-22 Created: 2016-12-22 Last updated: 2016-12-22Bibliographically approved

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Lind, KarinBarklem, Paul S.
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