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S stars in the Gaia era: stellar parameters and nucleosynthesis

Published online by Cambridge University Press:  07 March 2018

Sophie Van Eck ,
Drisya Karinkuzhi ,
Shreeya Shetye ,
Alain Jorissen ,
Stéphane Goriely ,
Lionel Siess ,
Thibault Merle  and
Bertrand Plez
Sophie Van Eck
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Drisya Karinkuzhi
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Shreeya Shetye
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected] Instituut voor Sterrenkunde (IvS), KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium
Alain Jorissen
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Stéphane Goriely
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Lionel Siess
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Thibault Merle
Affiliation:
Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium email: [email protected]
Bertrand Plez
Affiliation:
LUPM, Université Montpellier 2, CNRS, F-34095 Montpellier, France
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Abstract

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S stars are s-process and C-enriched (0.5<C/O<1) red giants. Their abundances can be determined thanks to a new grid of MARCS model atmospheres covering their whole parameter range. Detailed abundance determinations in intrinsic S stars (TP-AGB) and extrinsic S stars (binary masqueraders) can provide strong constraints on the s-process nucleosynthesis: in particular, the s-process temperature can be determined using zirconium and niobium abundances, independently of stellar evolution models. Synthetic spectra of dwarf S stars have been computed and will be sought for in spectroscopic survey data, constraining their luminosity thanks to Gaia parallaxes.

Keywords

Nuclear reactionsnucleosynthesisabundancesstars: AGB and post-AGBstars: atmospheresstars: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 352 - 353
Copyright
Copyright © International Astronomical Union 2018 

References

Gustafsson, B., Edvardsson, B., Eriksson, K., Jørgensen, U. G., Nordlund, Å & Plez, B., 2008, A&A, 486, 951–970 Google Scholar
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Raskin, G., Van Winckel, H., Hensberge, H., Jorissen, A., Lehmann, H. et al., 2011, A&A, 526, A69 Google Scholar
Neyskens, P., Van Eck, S., Jorissen, A., Goriely, S., Siess, L., & Plez, B., 2015, Nature, 517, 174 CrossRefGoogle Scholar