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Beryllium and boron in metal-poor stars

Published online by Cambridge University Press:  23 April 2010

Francesca Primas
Francesca Primas*
Affiliation:
European Southern Observatory, KarlSchwarzschild Strasse 2, D-85748, Garching b. München, Germany email: fprimas@eso.org
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Abstract

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Knowledge of lithium, beryllium, and boron abundances in stars of the Galactic halo and disk plays a major role in our understanding of Big Bang nucleosynthesis, cosmic-ray physics, and stellar interiors. 9Be and 10B are believed to originate entirely from spallation reactions in the interstellar medium (ISM) between α-particles and protons and heavy nuclei like carbon, nitrogen, and oxygen (CNO), whereas 11B may have an extra production channel via neutrino-spallation. Beryllium and boron are both observationally challenging, with their main resonant doublets falling respectively at 313 nm and at 250 nm. The advent of 8-10m class telescopes equipped with highly sensitive (in the near-UV/blue) spectrographs has opened up a new era of Be abundance studies. Here, I will review and discuss the most interesting results of recent observational campaigns in terms of formation and evolution of these two light elements.

Keywords

Galaxy: haloabundancesevolution – stars: Population IIabundancesatmospheresinteriors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 221 - 230
Copyright
Copyright © International Astronomical Union 2010

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