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3D NLTE modelling o...
3D NLTE modelling of Y and Eu : Centre-to-limb variation and solar abundances
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- Storm, N. (author)
- Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
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- Barklem, Paul (author)
- Uppsala universitet,Teoretisk astrofysik
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- Yakovleva, S. A. (author)
- Herzen Univ, Inst Phys, St Petersburg 191186, Russia.
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- Belyaev, A. K. (author)
- Herzen Univ, Inst Phys, St Petersburg 191186, Russia.
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- Palmeri, P. (author)
- Univ Mons UMONS, Phys At & Astrophys, B-7000 Mons, Belgium.
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- Quinet, P. (author)
- Univ Mons UMONS, Phys At & Astrophys, B-7000 Mons, Belgium.;Univ Liege, IPNAS, B-4000 Liege, Belgium.
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- Lodders, K. (author)
- Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO USA.;Washington Univ, McDonnell Ctr Space Sci, St Louis, MO USA.
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- Bergemann, M. (author)
- Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
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- Hoppe, R. (author)
- Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany.
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Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany Teoretisk astrofysik (creator_code:org_t)
- EDP Sciences, 2024
- 2024
- English.
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In: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 683
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Abstract
Subject headings
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- Context: Abundances of s- and r-process elements in Sun-like stars constrain nucleosynthesis in extreme astrophysical events, such as compact binary mergers and explosions of highly magnetised rapidly rotating massive stars.Aims: We measure solar abundances of yttrium (Y) and europium (Eu) using 3D non-local thermal equilibrium (NLTE) models. We use the model to determine the abundance of Y, and also explore the model's ability to reproduce the solar centre-to-limb variation of its lines. In addition, we determine the Eu abundance using solar disc-centre and integrated flux spectra.Methods: We developed an NLTE model of Eu and updated our model of Y with collisional data from detailed quantum-mechanical calculations. We used the IAG spatially resolved high-resolution solar spectra to derive the solar abundances of Y across the solar disc and of Eu for integrated flux and at disc centre using a set of carefully selected lines and a 3D radiation-hydrodynamics model of the solar atmosphere.Results: We find 3D NLTE solar abundances of A(Y)(3D NLTE) = 2.30 ± 0.03stat ± 0.07syst dex based on observations at all angles and A(Eu) = 0.57 ± 0.01stat ± 0.06syst dex based on the integrated flux and disc-centre intensity. 3D NLTE modelling offers the most consistent abundances across the solar disc, and resolves the problem of severe systematic bias in Y and Eu abundances inherent to 1D LTE, 1D NLTE, and 3D LTE modelling.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- atomic data
- line: formation
- methods: observational
- Sun: abundances
- Sun: atmosphere
Publication and Content Type
- ref (subject category)
- art (subject category)
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