Be-9 abundances in population II stars - Implications for light element nucleosynthesis

Details Be-9 abundances in population II stars - Implications for light element nucleosynthesis Be-9 abundances in population II stars - Implications for light element nucleosynthesis

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348l..57r&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 348, Jan. 10, 1990, p. L57-L60.

Astronomy and Astrophysics

Astrophysics

70

Beryllium 9, Big Bang Cosmology, Light Elements, Nuclear Astrophysics, Nuclear Fusion, Stellar Spectra, Abundance, Dwarf Stars

Scientific paper

Upper limits on the Be-9 abundances in four metal-deficient dwarfs were obtained by applying the spectrum synthesis technique to high-resolution spectra at 3130 A. The abundance of Be-9 is seen to track the iron deficiency rather than maintain a nearly uniform abundance as is seen for the neighboring light element, Li-7. The deficiency of Be-9 permits the cosmic-ray spallation contribution to the Li-7 abundance of HD 140283 to be stated as less than 1 percent. The very low abundance of Be-9 can be used to constrain recent nonuniform density models for the big bang, which predict significant primordial abundances for this element.

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