期刊
ASTRONOMY & ASTROPHYSICS
卷 635, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201936603
关键词
nuclear reactions; nucleosynthesis; abundances; stars; abundances; Galaxy; abundances; supernovae; general
资金
- Australian Research Council [FT160100028]
- European Union Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant [664931]
- EU COST Action [CA16117]
- CNES, Centre National d'Etudes Spatiales
- Collaborative Research centre, Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) [SFB 881]
- Australian Research Council [FT160100028] Funding Source: Australian Research Council
The abundance ratios of manganese to iron in late-type stars across a wide metallicity range place tight constraints on the astrophysical production sites of Fe-group elements. In this work, we investigate the chemical evolution of Mn in the Milky Way galaxy using high-resolution spectroscopic observations of stars in the Galactic disc and halo stars, as well as a sample of globular clusters. Our analysis shows that local thermodynamic equilibrium (LTE) leads to a strong imbalance in the ionisation equilibrium of Mn I and Mn II lines. Mn I produces systematically (up to 0.6 dex) lower abundances compared to the Mn II lines. Non-LTE (NLTE) radiative transfer satisfies the ionisation equilibrium across the entire metallicity range, of -3 less than or similar to [Fe/H] less than or similar to -1, leading to consistent abundances from both ionisation stages of the element. We compare the NLTE abundances with Galactic Chemical Evolution models computed using different sources of type Ia and type II supernova (SN Ia and SN II) yields. We find that a good fit to our observations can be obtained by assuming that a significant (similar to 75%) fraction of SNe Ia stem from a sub-Chandrasekhar (sub-M-ch) channel. While this fraction is larger than that found in earlier studies (similar to 50%), we note that we still require similar to 25% near-M-ch SNe Ia to obtain solar [Mn/Fe] at [Fe/H] = 0. Our new data also suggest higher SN II Mn yields at low metallicity than typically assumed in the literature.
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