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The Barium Isotopic Abundance in the Metal-Poor Star HD140283

Published online by Cambridge University Press:  05 March 2013

R. Collet ,
M. Asplund  and
P. E. Nissen
R. Collet*
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1317, D–85741 Garching b. München, Germany
M. Asplund
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1317, D–85741 Garching b. München, Germany
P. E. Nissen
Affiliation:
Department of Physics and Astronomy, University of Aarhus, DK–8000 Aarhus C, Denmark
*
CCorresponding author. Email: remo@mpa-garching.mpg.de
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Abstract

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We derive the mixture of odd to even barium isotopes in the atmosphere of the metal-poor subgiant HD140283 from the analysis of the Ba ii transition at 4554 Å in a high-resolution high signal-to-noise spectrum of the star. The detailed shape of this spectral line depends on the relative contributions of odd and even isotopes via isotopic and hyperfine splitting. We measure the fractional abundance of odd Ba isotopes by modelling the formation of the Ba ii 4554-Å line profile with the use of both a classical 1D hydrostatic and a 3D hydrodynamical model atmosphere of HD140283. We interpret the results in terms of contributions by the slow (s) and rapid (r) neutron-capture processes to the isotopic mix. While the result of the 1D analysis of the Ba ii feature indicates a 64 ± 36% contribution of the r-process to the isotopic mix, the 3D analysis points toward a mere 15 ± 34% contribution from this process, that is consistent with a solar-like mixture of barium isotopes.

Keywords

hydrodynamicsline: profilesstars: atmospheresstars: abundancesstars: individual: HD140283
Type
Observations
Information
Publications of the Astronomical Society of Australia , Volume 26 , Issue 3 , 2009 , pp. 330 - 334
Copyright
Copyright © Astronomical Society of Australia 2009

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