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The Galactic Evolution of Beryllium

Published online by Cambridge University Press:  25 May 2016

Ann Merchant Boesgaard
Ann Merchant Boesgaard*
Affiliation:
University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, Hi 96822 U.S.A.

Abstract

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The abundance of beryllium has been determined in unevolved stars over a range metal abundances in order to enhance our understanding of the chemical evolution of our Galaxy, cosmic-ray theory, and cosmology. Observations of 27 stars have been made with Keck I with HIRES at high spectral resolution (45,000) and high signal-to-noise ratios (60 - 110 typically). We find a remarkably linear relationship between log N(Be/H) and [Fe/H] with a slope of 0.96 (±0.04). Similarly, the relationship between log N(Be/H) and [O/H] is linear with a slope of 1.45 (±0.04). Beryllium increases at the same rate as Fe, but much faster than O. This provides constraints for and insights into models of Galactic chemical evolution. There is some evidence for an intrinsic spread in Be at a given [O/H] or [Fe/H]. There is no evidence of a plateau in Be at the lowest metallicities down to log N(Be/H) = —13.5.

Type
5. Abundance of Beryllium and Boron
Information
Symposium - International Astronomical Union , Volume 198: The Light Elements and their Evolution , 2000 , pp. 389 - 396
Copyright
Copyright © Astronomical Society of the Pacific 2000 

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