3D non-local thermodynamic equilibrium magnesium abundances reveal a distinct halo population
Magnesium is one of the most important elements in stellar physics as an electron donor; in Galactic archaeology, magnesium serves to distinguish different stellar populations. However, previous studies of Mg I and Mg II lines in metal-poor benchmark stars indicate that magnesium abundances inferred...
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| Hauptverfasser: | , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
August 2024
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| In: |
Astronomy and astrophysics
Year: 2024, Jahrgang: 688, Pages: 1-8 |
| ISSN: | 1432-0746 |
| DOI: | 10.1051/0004-6361/202450057 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202450057 Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2024/08/aa50057-24/aa50057-24.html 
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| Verfasserangaben: | T. Matsuno, A.M. Amarsi, M. Carlos, and P.E. Nissen |
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| 246 | 3 | 3 | |a Three D non-local thermodynamic equilibrium magnesium abundances reveal a distinct halo population |
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| 520 | |a Magnesium is one of the most important elements in stellar physics as an electron donor; in Galactic archaeology, magnesium serves to distinguish different stellar populations. However, previous studies of Mg I and Mg II lines in metal-poor benchmark stars indicate that magnesium abundances inferred from one-dimensional (1D), hydrostatic models of stellar atmospheres, both with and without the local thermodynamic equilibrium (LTE) approximation, can be problematic. Here, we present three-dimensional (3D) non-LTE calculations for magnesium in FG-type dwarfs and provide corrections for 1D-LTE abundances. 3D non-LTE corrections reduce the ionisation imbalances in the benchmark metal-poor stars HD84937 and HD140283 from −0.16 dex and −0.27 dex in 1D LTE to just −0.02 dex and −0.09 dex, respectively. We applied our abundance corrections to 1D LTE literature results for stars in the thin disc, thick disc, α-rich halo, and α-poor halo. We observed that 3D non-LTE results had a richer substructure in [Mg/Fe] − [Fe/H] in the α-poor halo, revealing two sub-populations at the metal-rich end. These two sub-populations also differ in kinematics, supporting the astro-physical origin of the separation. While the more magnesium-poor sub-population is likely to be debris from a massive accreted galaxy, Gaia-Enceladus, the other sub-population may be related to a previously identified group of stars, called Eos. The additional separation in [Mg/Fe] suggests that previous Mg abundance measurements may have been imprecise due to the 1D and LTE approximations, highlighting the importance of 3D non-LTE modelling. | ||
| 700 | 1 | |a Amarsi, A. M. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Carlos, M. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Nissen, P. E. |e VerfasserIn |4 aut | |
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