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High-precision abundances of elements in stars with asteroseismic ages

Published online by Cambridge University Press:  02 August 2018

P. E. Nissen ,
V. Silva Aguirre ,
J. Christensen-Dalsgaard ,
R. Collet ,
F. Grundahl  and
D. Slumstrup
P. E. Nissen
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
V. Silva Aguirre
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
J. Christensen-Dalsgaard
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
R. Collet
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
F. Grundahl
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
D. Slumstrup
Affiliation:
Stellar Astrophysics Centre, Dept. of Physics and Astronomy, Aarhus University, Denmark email: pen@phys.au.dk
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Abstract

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High-precision abundances of elements have been derived from HARPS-N spectra of F and G main-sequence stars having ages determined from oscillation frequencies delivered by the Kepler mission. The tight relations between abundance ratios of refractory elements, e.g., [Mg/Fe] and [Y/Mg], and stellar age previously found for solar twin stars are confirmed. These relations provide new information on nucleosynthesis and Galactic evolution. Abundance ratios between volatile and refractory elements, e.g., [C/Fe] and [O/Fe], show on the other hand a significant scatter at a given age, which may be related to planet-star interactions. This is a potential problem for chemical tagging studies.

Keywords

Stars: abundancesStars: oscillationsPlanet-star interactionGalaxy: diskGalaxy: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 166 - 169
Copyright
Copyright © International Astronomical Union 2018 

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