| Issue |
EAS Publications Series
Volume 71-72, 2015
The Physics of Evolved Stars: A Conference Dedicated to the Memory of Olivier Chesneau
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|---|---|---|
| Page(s) | 343 - 344 | |
| Section | Modeling, Evolution | |
| DOI | https://doi.org/10.1051/eas/1571081 | |
| Published online | 01 December 2015 | |
E. Lagadec, F. Millour and T. Lanz (eds)
EAS Publications Series, 71–72 (2015) 343-344
s-Process Abundances in Binary Stars With White Dwarfs
1 Institut d*Astronomie et d*Astrophysique, Université Libre de Bruxelles, Belgium
2 Institute of Astronomy, University of Cambridge, UK
3 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Belgium
The enrichment of barium stars in s-process elements is known to be due to pollution by mass transfer from an asymptotic giant branch (AGB) companion star, now an extincted C-O white-dwarf (McClure et al. [4]; Gray et al. [1]). We investigate the relationship between the level of enrichment in s-process elements in the barium star and the mass of its white dwarf (WD) companion. It is expected that helium WDs, which have masses smaller than about 0.5 M⊙ and whose progenitor never reached the AGB phase, should not pollute with s-process elements their giant companion. That companion should thus never turn into a barium star. Our results conform to the expectation that binary systems with WD companions less massive than 0.5 M⊙ do not host barium stars.
© EAS, EDP Sciences, 2015