Additional fluorine abundance determinations in evolved stars
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AuthorAbia Ladrón De Guevara, Carlos Antonio; Cristallo, S.; Cunha, K.; Laverny, P. de; Smith, V. V.
Abia, C., Cristallo, S., Cunha, K., De Laverny, P., & Smith, V. V. (2019). Additional fluorine abundance determinations in evolved stars. Astronomy & Astrophysics, 625, A40.
SponsorshipThis work was partially supported by the Spanish grant AYA2015-63588-P within the European Founds for Regional Development (FEDER).
We present new fluorine abundance measurements for a sample of carbon-rich asymptotic giant branch (AGB) stars and two other metal-poor evolved stars of Ba/CH types. The abundances are derived from IR, K-band, high-resolution spectra obtained using GEMINI-S/Phoenix and TNG/Giano-b. Our sample includes an extragalactic AGB carbon star belonging to the Sagittarius dSph galaxy. The metallicity of our stars ranges from [Fe/H] = 0:0 down to -1:4 dex. The new measurements, together with those previously derived in similar stars, show that normal (N-type) and SC-type AGB carbon stars of near solar metallicity present similar F enhancements, discarding previous hints that suggested that SC-type stars have larger enhancements. These mild F enhancements are compatible with current chemical-evolution models pointing out that AGB stars, although relevant, are not the main sources of this element in the solar neighbourhood. Larger [F/Fe] ratios are found for lower-metallicity stars. This is confirmed by theory. We highlight a tight relation between the [F/hsi] ratio and the average s-element enhancement [hsi/Fe] for stars with [Fe/H] > -0:5, which can be explained by the current state-of-the-art low-mass AGB models assuming an extended 13C pocket. For stars with [Fe/H] < -0:5, discrepancies between observations and model predictions still exist. We conclude that the mechanism of F production in AGB stars needs further scrutiny and that simultaneous F and s-element measurements in a larger number of metal-poor AGB stars are needed to better constrain the models.