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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
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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2010

References

Boesgaard, A. M. 2007, ApJ, 667, 1196CrossRefGoogle Scholar
Boesgaard, A. M. & King, J. R. 2002, ApJ, 565, 587CrossRefGoogle Scholar
Boesgaard, A. M. & Novicki, M. C. 2006, ApJ, 641, 1122CrossRefGoogle Scholar
Boesgaard, A. M., Armengaud, E., & King, J. R. 2003a, ApJ, 582, 410CrossRefGoogle Scholar
Boesgaard, A. M., Armengaud, E., & King, J. R. 2003b, ApJ, 583, 955CrossRefGoogle Scholar
Boesgaard, A. M., Armengaud, E., & King, J. R. 2004a, ApJ, 605, 864CrossRefGoogle Scholar
Boesgaard, A. M., Armengaud, E., King, J. R., Deliyannis, C. P., & Stephens, A. 2004b, ApJ, 613, 1202CrossRefGoogle Scholar
Boesgaard, A. M., Deliyannis, C. P., King, J. R., Ryan, S. G., Vogt, S. S., & Beers, T. C. 1999, AJ, 117, 1549CrossRefGoogle Scholar
Boesgaard, A. M., Stephens, A., & Deliyannis, C. P. 2005, ApJ, 633, 398CrossRefGoogle Scholar
Gratton, R. G., Carretta, E., Claudi, R, Lucatello, S., & Barbien, M. 2003, A&A, 404, 187Google Scholar
Grevesse, N. & Sauval, A. J. 1998, Space Sci. Rev., 85, 161CrossRefGoogle Scholar
Pasquini, L., Galli, D., Gratton, R. G., Bonifacio, P., Randich, S., & Valle, G. 2005, A&A (Letters), 436, 57Google Scholar
Pinsonneault, M. H., Deliyannis, C. P., & Demarque, P. 1992, ApJS, 78, 179CrossRefGoogle Scholar
Pinsonneault, M. H., Steigman, G., Walker, T. P., & Narayanan, V. K. 2002, ApJ, 574, 398CrossRefGoogle Scholar
Pinsonneault, M. H., Walker, T. P., Steigman, G., & Narayanan, V. K. 1999, ApJ, 527, 180CrossRefGoogle Scholar
Primas, F., Asplund, M., Nissen, P. E., & Hill, V. 2000a, A&A (Letters), 364, 42Google Scholar
Primas, F., Asplund, M, Bonifacio, P., & Hill, V. 2000b, A&A, 362, 666Google Scholar
Rich, J. A. & Boesgaard, A. M. 2009, ApJ, 701, 1519CrossRefGoogle Scholar
Ryan, S. G., Beers, T. C., Kajino, T., & Rosolankova, K. 2001, ApJ, 547, 231CrossRefGoogle Scholar
Ryan, S. G., Gregory, S. G., Kolb, U., Beers, T. C., & Kajino, T. 2002, ApJ, 571, 501CrossRefGoogle Scholar
Smiljanic, R., Pasquini, L., Bonifacio, P., Galli, D., Gratton, R. G., Randich, S., & Wolff, B. 2009, A&A, 499, 103Google Scholar
Vogt, S. S. et al. 1994, SPIE, 2198, 362Google Scholar
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New Beryllium results in halo stars from Keck/HIRES spectra
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