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New Beryllium results in halo stars from Keck/HIRES spectra

Published online by Cambridge University Press:  23 April 2010

Ann Merchant Boesgaard ,
Jeffrey A. Rich ,
Emily M. Levesque  and
Brendan P. Bowler
Ann Merchant Boesgaard
Affiliation:
University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A. email: boes@ifa.hawaii.edu, jrich@ifa.hawaii.edu, emsque@ifa.hawaii.edu, bpbowler@ifa.hawaii.edu
Jeffrey A. Rich
Affiliation:
University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A. email: boes@ifa.hawaii.edu, jrich@ifa.hawaii.edu, emsque@ifa.hawaii.edu, bpbowler@ifa.hawaii.edu
Emily M. Levesque
Affiliation:
University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A. email: boes@ifa.hawaii.edu, jrich@ifa.hawaii.edu, emsque@ifa.hawaii.edu, bpbowler@ifa.hawaii.edu
Brendan P. Bowler
Affiliation:
University of Hawaii, Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, U.S.A. email: boes@ifa.hawaii.edu, jrich@ifa.hawaii.edu, emsque@ifa.hawaii.edu, bpbowler@ifa.hawaii.edu
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Abstract

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We have obtained high-resolution, high signal-to-noise Keck spectra to determine Be abundances in over 100 stars in the Galactic halo. The stellar metallicities range from [Fe/H] = −0.50 to −3.50. Using this large sample, we have examined the trends of Be with Fe and Be with O. We find a real dispersion in Be at a given [O/H] that indicates that Be may not be a good cosmochronometer. Our results indicate that the dominant production mechanism for Be changes as the Galaxy ages. In the early eras of the Galaxy, when massive stars become supernovae, Be is produced from the acceleration of energetic CNO atoms which bombard protons in the vicinity of supernovae. Later spallation reactions occur as high energy protons bombard CNO atoms in the interstellar gas. The change occurs near [Fe/H] = −2.2. We have found that Be is deficient in Li-deficient halo stars, which favors the blue straggler analog hypothesis.

Keywords

Stars: abundancesPopulation IIkinematicslate-type – Galaxy: halo
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 231 - 236
Copyright
Copyright © International Astronomical Union 2010

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