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Probing stellar evolution with S stars and Gaia

Published online by Cambridge University Press:  30 December 2019

S. Shetye Open the ORCID record for S. Shetye [Opens in a new window] ,
S. Van Eck ,
A. Jorissen ,
H. Van Winckel ,
L. Siess  and
S. Goriely
S. Shetye
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: Shreeya.Shetye@ulb.ac.be Instituut voor Sterrenkunde (IvS), KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
S. Van Eck
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: Shreeya.Shetye@ulb.ac.be
A. Jorissen
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: Shreeya.Shetye@ulb.ac.be
H. Van Winckel
Affiliation:
Instituut voor Sterrenkunde (IvS), KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
L. Siess
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: Shreeya.Shetye@ulb.ac.be
S. Goriely
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: Shreeya.Shetye@ulb.ac.be
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Abstract

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S-type stars are late-type giants enhanced with s-process elements originating either from nucleosynthesis during the Asymptotic Giant Branch (AGB) or from a pollution by a binary companion. The former are called intrinsic S stars, and the latter extrinsic S stars. The intrinsic S stars are on the AGB and have undergone third dredge-up events. The atmospheric parameters of S stars are more numerous than those of M-type giants (C/O ratio and s-process abundances affect the thermal structure and spectral synthesis), and hence they are more difficult to derive. These atmospheric parameters are also entangled within each other. Nevertheless, high-resolution spectroscopic data of S stars combined with the Gaia Data Release 2 (GDR2) parallaxes and with the MARCS model atmospheres for S-type stars were used to derive effective temperatures, surface gravities, and luminosities. These parameters not only allow to locate the intrinsic and extrinsic S stars in the Hertzsprung-Russell (HR) diagram but also allow the accurate abundance analysis of the s-process elements.

Keywords

S starsAGB starss-process nucleosynthesisHR diagram
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 69 - 72
Copyright
© International Astronomical Union 2019 

Footnotes

†

This work has made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

References

De Smedt, K. et al. 2015, A&A, 583, A56 Google Scholar
Collaboration, Gaia 2016, A&A, 595, A2 Google Scholar
Collaboration, Gaia 2018, A&A, 616A, 1G Google Scholar
Goriely, S. and Siess, L. 2018, A&A, 609, A29 Google Scholar
Iben, Jr. , I. and Renzini, A. 1983, ARA&A, 21, 271 CrossRefGoogle Scholar
Jorissen, A. et al. 1993, A&A, 271, 463 Google Scholar
Karakas, A. I. and Lugaro, M. 2016, ApJ, 825, 26 CrossRefGoogle Scholar
Merrill, P. W. 1922, ApJ, 56, 457M CrossRefGoogle Scholar
Merrill, P. W. 1952, ApJ, 116, 21 CrossRefGoogle Scholar
Raskin, G. et al. 2011, A&A, 526, A69 Google Scholar
Siess, L. and Arnould, M. 2008, A&A, 489, 395 Google Scholar
Smith, V. V. and Lambert, D. L. 1986, ApJ, 311, 843 CrossRefGoogle Scholar
Smith, V. V. and Lambert, D. L. 1990, ApJS, 72, 387 CrossRefGoogle Scholar
Stephenson, C. B. 1984, Publications of the Warner & Swasey Observatory, 3, 1 Google Scholar
Van Eck, S. et al. 2017, A&A, 601, A10 Google Scholar