High-resolution spectroscopic analysis of four unevolved barium stars
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| Format: | Preprint |
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2024
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| author | Roriz, M. P. Holanda, N. da Conceição, L. V. Junqueira, S. Drake, N. A. Sonally, A. Pereira, C. B. |
| author_facet | Roriz, M. P. Holanda, N. da Conceição, L. V. Junqueira, S. Drake, N. A. Sonally, A. Pereira, C. B. |
| contents | A classical Local Thermodynamic Equilibrium analysis, based on high-resolution spectroscopic data, is performed for a sample of three potential barium dwarf candidates and one star already recognized as such. We derived their atmospheric parameters, estimated their masses and luminosities, and determined chemical abundances for a set of 21 elements, including CNO. Some elemental abundances are derived for the first time in HD~15096, HD~37792, and HD~141804. The program stars are dwarfs/subgiants with metallicities typical of disc stars, exhibiting moderate carbon enhancements, with $\rm{[C/Fe]}$ ratios ranging from $+0.29$ to $+0.66$ dex, and high levels of \textit{slow} neutron-capture ($s$-process) elements, with $\rm{[\textit{s}/Fe]}\gtrsim +1.0$~dex. As spectroscopic binaries, their peculiarities are attributable to mass transfer events. The observed neutron-capture patterns of were individually compared with two sets of $s$-process nucleosynthesis models (Monash and {\sc fruity}), yielding dilution factors and masses estimates for the former polluting Asymptotic Giant Branch stars. Low-mass ($\lesssim 3.0~\rm{M}_{\odot}$) models successfully reproduce the observations. In addition, we estimated mean neutron exposures of the order of 0.6 -- 0.7 mb$^{-1}$ for the $s$-processed material observed in their envelopes. Applying an empirical initial-final mass relation, we constraint in $\sim 0.7\,\textrm{M}_{\odot}$ the mass of their dim white-dwarf companions. Moreover, our kinematic study revealed that the program stars are members of the thin disk, with probabilities greater than 70\%. Hence, we identified HD~15096 and HD~37792 as new barium dwarfs and confirmed that HD~141804 is a barium dwarf. Thus, the number of barium dwarfs identified in the literature from high-resolution spectroscopy increases to 71 objects. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2402_14709 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | High-resolution spectroscopic analysis of four unevolved barium stars Roriz, M. P. Holanda, N. da Conceição, L. V. Junqueira, S. Drake, N. A. Sonally, A. Pereira, C. B. Solar and Stellar Astrophysics A classical Local Thermodynamic Equilibrium analysis, based on high-resolution spectroscopic data, is performed for a sample of three potential barium dwarf candidates and one star already recognized as such. We derived their atmospheric parameters, estimated their masses and luminosities, and determined chemical abundances for a set of 21 elements, including CNO. Some elemental abundances are derived for the first time in HD~15096, HD~37792, and HD~141804. The program stars are dwarfs/subgiants with metallicities typical of disc stars, exhibiting moderate carbon enhancements, with $\rm{[C/Fe]}$ ratios ranging from $+0.29$ to $+0.66$ dex, and high levels of \textit{slow} neutron-capture ($s$-process) elements, with $\rm{[\textit{s}/Fe]}\gtrsim +1.0$~dex. As spectroscopic binaries, their peculiarities are attributable to mass transfer events. The observed neutron-capture patterns of were individually compared with two sets of $s$-process nucleosynthesis models (Monash and {\sc fruity}), yielding dilution factors and masses estimates for the former polluting Asymptotic Giant Branch stars. Low-mass ($\lesssim 3.0~\rm{M}_{\odot}$) models successfully reproduce the observations. In addition, we estimated mean neutron exposures of the order of 0.6 -- 0.7 mb$^{-1}$ for the $s$-processed material observed in their envelopes. Applying an empirical initial-final mass relation, we constraint in $\sim 0.7\,\textrm{M}_{\odot}$ the mass of their dim white-dwarf companions. Moreover, our kinematic study revealed that the program stars are members of the thin disk, with probabilities greater than 70\%. Hence, we identified HD~15096 and HD~37792 as new barium dwarfs and confirmed that HD~141804 is a barium dwarf. Thus, the number of barium dwarfs identified in the literature from high-resolution spectroscopy increases to 71 objects. |
| title | High-resolution spectroscopic analysis of four unevolved barium stars |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2402.14709 |