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Binary interaction along the RGB: The Barium Star perspective

Published online by Cambridge University Press:  30 December 2019

A. Escorza Open the ORCID record for A. Escorza [Opens in a new window] ,
L. Siess ,
D. Karinkuzhi ,
H. M. J. Boffin ,
A. Jorissen  and
H. van Winckel
A. Escorza
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium email: [email protected] Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Campus Plaine C.P. 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium
L. Siess
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Campus Plaine C.P. 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium F.R.S.-FNRS, Belgium
D. Karinkuzhi
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Campus Plaine C.P. 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium
H. M. J. Boffin
Affiliation:
ESO, Garching bei München, Germany
A. Jorissen
Affiliation:
Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, Campus Plaine C.P. 226, Boulevard du Triomphe, B-1050 Bruxelles, Belgium
H. van Winckel
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium email: [email protected]
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Abstract

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Barium (Ba) stars form via mass-transfer in binary systems, and can subsequently interact with their white dwarf companion in a second stage of binary interaction. We used observations of main-sequence Ba systems as input for our evolutionary models, and try to reproduce the orbits of the Ba giants. We show that to explain short and sometimes eccentric orbits, additional interaction mechanisms are needed along the RGB.

Keywords

stars: binariesstars: evolution
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. 394 - 395
Copyright
© International Astronomical Union 2019 

References

Bailer-Jones, C. A. L., Rybizki, J., Fouesneau, M., et al. 2018, AJ, 156, 58 CrossRefGoogle Scholar
Escorza, A., Boffin, H. M. J., Jorissen, A., et al. 2017, A&A, 608, A100 CrossRefGoogle Scholar
Jorissen, A., Van Eck, S., Van Winckel, H., et al. 2016, A&A, 586, A158 CrossRefGoogle Scholar
Lindegren, L., Lammers, U., Bastian, U., et al. 2016, A&A, 595, A4 Google Scholar
McClure, R. D. 1984, PASP, 96, 117 CrossRefGoogle Scholar
Nie, J. D., Wood, P. R., & Nicholls, C. P. 2017, ApJ, 835, 209 CrossRefGoogle Scholar
Siess, L. 2006, A&A, 448, 717 CrossRefGoogle Scholar
Siess, L., Izzard, R. G., Davis, P. J., & Deschamps, R. 2013, A&A, 550, A100 CrossRefGoogle Scholar
Tout, C. A., & Eggleton, P. P. 1988, MNRAS, 231, 823 CrossRefGoogle Scholar