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Beryllium abundances in metal-rich stars

Published online by Cambridge University Press:  23 April 2010

Ruth C. Peterson
Ruth C. Peterson*
Affiliation:
UCO/Lick Observatories and Astrophysical Advances email: [email protected]
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Abstract

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In metal-rich stars as cool as the Sun, beryllium abundance determinations are difficult due to heavy line blanketing in the near-UV 3130 Å region where the accessible Be II lines reside. We can now attempt such determinations based on improved lists of atomic line identifications and gf-values in the near-UV. Here we report Be determinations for three metal-rich A, F, and G stars plus three solar-metallicity standards. All six stars have beryllium-to-hydrogen ratios at or below solar. More such determinations would provide stronger constraints on trends in Be abundance with temperature, metallicity, and age.

Keywords

Stars: abundancesindividual (HD 61421, HD 72660, HD 165341, HD 179949, HD 217107)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 349 - 350
Copyright
Copyright © International Astronomical Union 2010

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