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Barium stars as tracers of s-process nucleosynthesis in AGB stars : I. 28 stars with independently derived AGB mass. / Cseh, B.; Világos, B.; Roriz, M. P.; Pereira, C. B.; D'Orazi, V.; Karakas, A. I.; Soós, B.; Drake, N. A.; Junqueira, S.; Lugaro, M.

In: Astronomy and Astrophysics, Vol. 660, A128, 01.04.2022.

Research output: Contribution to journalArticlepeer-review

Harvard

Cseh, B, Világos, B, Roriz, MP, Pereira, CB, D'Orazi, V, Karakas, AI, Soós, B, Drake, NA, Junqueira, S & Lugaro, M 2022, 'Barium stars as tracers of s-process nucleosynthesis in AGB stars: I. 28 stars with independently derived AGB mass', Astronomy and Astrophysics, vol. 660, A128. https://doi.org/10.1051/0004-6361/202142468

APA

Cseh, B., Világos, B., Roriz, M. P., Pereira, C. B., D'Orazi, V., Karakas, A. I., Soós, B., Drake, N. A., Junqueira, S., & Lugaro, M. (2022). Barium stars as tracers of s-process nucleosynthesis in AGB stars: I. 28 stars with independently derived AGB mass. Astronomy and Astrophysics, 660, [A128]. https://doi.org/10.1051/0004-6361/202142468

Vancouver

Cseh B, Világos B, Roriz MP, Pereira CB, D'Orazi V, Karakas AI et al. Barium stars as tracers of s-process nucleosynthesis in AGB stars: I. 28 stars with independently derived AGB mass. Astronomy and Astrophysics. 2022 Apr 1;660. A128. https://doi.org/10.1051/0004-6361/202142468

Author

Cseh, B. ; Világos, B. ; Roriz, M. P. ; Pereira, C. B. ; D'Orazi, V. ; Karakas, A. I. ; Soós, B. ; Drake, N. A. ; Junqueira, S. ; Lugaro, M. / Barium stars as tracers of s-process nucleosynthesis in AGB stars : I. 28 stars with independently derived AGB mass. In: Astronomy and Astrophysics. 2022 ; Vol. 660.

BibTeX

@article{be9fe706096446af96107da877a2ad0a,
title = "Barium stars as tracers of s-process nucleosynthesis in AGB stars: I. 28 stars with independently derived AGB mass",
abstract = "Context. Barium (Ba) stars are polluted by material enriched in the slow neutron capture (s-process) elements synthesised in the interior of their former asymptotic giant branch (AGB) companion star, which is now a white dwarf. Aims. We aim to compare individual Ba star abundance patterns to AGB nucleosynthesis model predictions to verify if the AGB model mass is compatible with independently derived AGB mass, which was previously estimated using binary parameters and Gaia parallax data. Methods. We selected a sample of 28 Ba stars for which both self-consistent spectroscopic observation and analysis were performed and, additionally, stellar mass determinations, via positioning the star on the Hertzsprung-Russell (HR) diagram and comparing with evolutionary tracks are available. For this sample of stars, we considered both previously (Y, Zr, Ce, and Nd) and recently derived (Rb, Sr, Nb, Mo, Ru, La, Sm, and Eu) elemental abundances. Then, we performed a detailed comparison of these s-process elemental abundances to different AGB nucleosynthesis models from the Monash and the FRUITY theoretical data sets. We simplified the binary mass transfer by calculating dilution factors to match the [Ce/Fe] value of each star when using different AGB nucleosynthesis models, and we then compared the diluted model abundances to the complete Ba-star abundance pattern. Results. Our comparison confirms that low-mass (with initial masses roughly in the range 2-3 M·), non-rotating AGB stellar models with 13C as the main neutron source are the polluters of the vast majority of the considered Ba stars. Out of the 28 stars, in 21 cases the models are in good agreement with both the determined abundances and the independently derived AGB mass, although in 16 cases higher observed abundances of Nb, Ru, Mo, and/or Nd, Sm than predicted were present. For three stars, we obtain a match to the abundances only by considering models with masses lower than those independently determined. Finally, four stars show much higher first s-process peak abundance values than the model predictions, which may represent the signature of a physical (e.g. mixing) and/or nucleosynthetic process that is not represented in the set of models considered here.",
keywords = "Abundances, Nuclear reactions, Nucleosynthesis, Stars: AGB and post-AGB, Stars: chemically peculiar",
author = "B. Cseh and B. Vil{\'a}gos and Roriz, {M. P.} and Pereira, {C. B.} and V. D'Orazi and Karakas, {A. I.} and B. So{\'o}s and Drake, {N. A.} and S. Junqueira and M. Lugaro",
note = "Publisher Copyright: {\textcopyright} 2022 ESO.",
year = "2022",
month = apr,
day = "1",
doi = "10.1051/0004-6361/202142468",
language = "English",
volume = "660",
journal = "ASTRONOMY & ASTROPHYSICS",
issn = "0004-6361",
publisher = "EDP Sciences",

}

RIS

TY - JOUR

T1 - Barium stars as tracers of s-process nucleosynthesis in AGB stars

T2 - I. 28 stars with independently derived AGB mass

AU - Cseh, B.

AU - Világos, B.

AU - Roriz, M. P.

AU - Pereira, C. B.

AU - D'Orazi, V.

AU - Karakas, A. I.

AU - Soós, B.

AU - Drake, N. A.

AU - Junqueira, S.

AU - Lugaro, M.

N1 - Publisher Copyright: © 2022 ESO.

PY - 2022/4/1

Y1 - 2022/4/1

N2 - Context. Barium (Ba) stars are polluted by material enriched in the slow neutron capture (s-process) elements synthesised in the interior of their former asymptotic giant branch (AGB) companion star, which is now a white dwarf. Aims. We aim to compare individual Ba star abundance patterns to AGB nucleosynthesis model predictions to verify if the AGB model mass is compatible with independently derived AGB mass, which was previously estimated using binary parameters and Gaia parallax data. Methods. We selected a sample of 28 Ba stars for which both self-consistent spectroscopic observation and analysis were performed and, additionally, stellar mass determinations, via positioning the star on the Hertzsprung-Russell (HR) diagram and comparing with evolutionary tracks are available. For this sample of stars, we considered both previously (Y, Zr, Ce, and Nd) and recently derived (Rb, Sr, Nb, Mo, Ru, La, Sm, and Eu) elemental abundances. Then, we performed a detailed comparison of these s-process elemental abundances to different AGB nucleosynthesis models from the Monash and the FRUITY theoretical data sets. We simplified the binary mass transfer by calculating dilution factors to match the [Ce/Fe] value of each star when using different AGB nucleosynthesis models, and we then compared the diluted model abundances to the complete Ba-star abundance pattern. Results. Our comparison confirms that low-mass (with initial masses roughly in the range 2-3 M·), non-rotating AGB stellar models with 13C as the main neutron source are the polluters of the vast majority of the considered Ba stars. Out of the 28 stars, in 21 cases the models are in good agreement with both the determined abundances and the independently derived AGB mass, although in 16 cases higher observed abundances of Nb, Ru, Mo, and/or Nd, Sm than predicted were present. For three stars, we obtain a match to the abundances only by considering models with masses lower than those independently determined. Finally, four stars show much higher first s-process peak abundance values than the model predictions, which may represent the signature of a physical (e.g. mixing) and/or nucleosynthetic process that is not represented in the set of models considered here.

AB - Context. Barium (Ba) stars are polluted by material enriched in the slow neutron capture (s-process) elements synthesised in the interior of their former asymptotic giant branch (AGB) companion star, which is now a white dwarf. Aims. We aim to compare individual Ba star abundance patterns to AGB nucleosynthesis model predictions to verify if the AGB model mass is compatible with independently derived AGB mass, which was previously estimated using binary parameters and Gaia parallax data. Methods. We selected a sample of 28 Ba stars for which both self-consistent spectroscopic observation and analysis were performed and, additionally, stellar mass determinations, via positioning the star on the Hertzsprung-Russell (HR) diagram and comparing with evolutionary tracks are available. For this sample of stars, we considered both previously (Y, Zr, Ce, and Nd) and recently derived (Rb, Sr, Nb, Mo, Ru, La, Sm, and Eu) elemental abundances. Then, we performed a detailed comparison of these s-process elemental abundances to different AGB nucleosynthesis models from the Monash and the FRUITY theoretical data sets. We simplified the binary mass transfer by calculating dilution factors to match the [Ce/Fe] value of each star when using different AGB nucleosynthesis models, and we then compared the diluted model abundances to the complete Ba-star abundance pattern. Results. Our comparison confirms that low-mass (with initial masses roughly in the range 2-3 M·), non-rotating AGB stellar models with 13C as the main neutron source are the polluters of the vast majority of the considered Ba stars. Out of the 28 stars, in 21 cases the models are in good agreement with both the determined abundances and the independently derived AGB mass, although in 16 cases higher observed abundances of Nb, Ru, Mo, and/or Nd, Sm than predicted were present. For three stars, we obtain a match to the abundances only by considering models with masses lower than those independently determined. Finally, four stars show much higher first s-process peak abundance values than the model predictions, which may represent the signature of a physical (e.g. mixing) and/or nucleosynthetic process that is not represented in the set of models considered here.

KW - Abundances

KW - Nuclear reactions

KW - Nucleosynthesis

KW - Stars: AGB and post-AGB

KW - Stars: chemically peculiar

UR - http://www.scopus.com/inward/record.url?scp=85129217495&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202142468

DO - 10.1051/0004-6361/202142468

M3 - Article

AN - SCOPUS:85129217495

VL - 660

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

M1 - A128

ER -

ID: 99849150