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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 03851naa a2200421 4500 | |
| 001 | oai:lup.lub.lu.se:3e57348a-9852-45da-99c2-4d83f27714e7 | |
| 003 | SwePub | |
| 008 | 171128s2017 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://lup.lub.lu.se/record/3e57348a-9852-45da-99c2-4d83f27714e72 URI |
| 024 | 7 | a https://doi.org/10.3847/1538-4357/aa88cb2 DOI |
| 040 | a (SwePub)lu | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a art2 swepub-publicationtype |
| 072 | 7 | a ref2 swepub-contenttype |
| 100 | 1 | a Bergemann, Mariau Max Planck Institute for Astronomy4 aut |
| 245 | 1 0 | a Non-local Thermodynamic Equilibrium Stellar Spectroscopy with 1D and 〈3〉 Models. I. Methods and Application to Magnesium Abundances in Standard Stars |
| 264 | c 2017-09-15 | |
| 264 | 1 | b American Astronomical Society,c 2017 |
| 520 | a We determine Mg abundances in six Gaia benchmark stars using theoretical one-dimensional (1D) hydrostatic model atmospheres, as well as temporally and spatially averaged three-dimensional (〈3D〉) model atmospheres. The stars cover a range of Teff from 4700 to 6500 K, log g from 1.6 to 4.4 dex, and [Fe H] from -3.0 dex to solar. Spectrum synthesis calculations are performed in local thermodynamic equilibrium (LTE) and in non-LTE (NLTE) using the oscillator strengths recently published by Pehlivan Rhodin et al. We find that: (a) Mg abundances determined from the infrared spectra are as accurate as the optical diagnostics, (b) the NLTE effects on Mg I line strengths and abundances in this sample of stars are minor (although for a few Mg I lines the NLTE effects on abundance exceed 0.6 dex in 〈3D〉 and 0.1 dex in 1D, (c) the solar Mg abundance is 7.56 ± 0.05 dex (total error), in excellent agreement with the Mg abundance measured in CI chondritic meteorites, (d) the 1D NLTE and 〈3D〉 NLTE approaches can be used with confidence to analyze optical Mg I lines in spectra of dwarfs and sub-giants, but for red giants the Mg I 5711 line should be preferred, (e) low-excitation Mg I lines are sensitive to the atmospheric structure; for these lines, LTE calculations with 〈3D〉 models lead to significant systematic abundance errors. The methods developed in this work will be used to study Mg abundances of a large sample of stars in the next paper in the series. | |
| 650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
| 653 | a galaxies: abundances | |
| 653 | a line: formation | |
| 653 | a radiative transfer | |
| 653 | a stars: abundances | |
| 653 | a stars: late-type | |
| 700 | 1 | a Collet, Remou Australian National University,Aarhus University4 aut |
| 700 | 1 | a Amarsi, Anish M.u Max Planck Institute for Astronomy,Australian National University4 aut |
| 700 | 1 | a Kovalev, Mikhailu Max Planck Institute for Astronomy4 aut |
| 700 | 1 | a Ruchti, Gregu Lund University,Lunds universitet,Astronomi - Har omorganiserats,Institutionen för astronomi och teoretisk fysik - Har omorganiserats,Naturvetenskapliga fakulteten,Lund Observatory - Has been reorganised,Department of Astronomy and Theoretical Physics - Has been reorganised,Faculty of Science4 aut0 (Swepub:lu)astr-grh |
| 700 | 1 | a Magic, Zazraltu University of Copenhagen,Natural History Museum of Denmark4 aut |
| 710 | 2 | a Max Planck Institute for Astronomyb Australian National University4 org |
| 773 | 0 | t Astrophysical Journald : American Astronomical Societyg 847:1q 847:1x 0004-637Xx 1538-4357 |
| 856 | 4 | u http://dx.doi.org/10.3847/1538-4357/aa88cby FULLTEXT |
| 856 | 4 | u https://arxiv.org/pdf/1612.07355.pdf |
| 856 | 4 8 | u https://lup.lub.lu.se/record/3e57348a-9852-45da-99c2-4d83f27714e7 |
| 856 | 4 8 | u https://doi.org/10.3847/1538-4357/aa88cb |
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