A Differential Abundance Analysis of Very Metal-poor Stars

Citation data:

The Astrophysical Journal, ISSN: 1538-4357, Vol: 838, Issue: 2

Publication Year:
2017
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Repository URL:
https://digitalcommons.dartmouth.edu/facoa/2130
DOI:
10.3847/1538-4357/aa62a2
Author(s):
O'Malley, Erin M; McWilliam, Andrew; Chaboyer, Brian; Thompson, Ian
Publisher(s):
American Astronomical Society
Tags:
Physics and Astronomy; Earth and Planetary Sciences; astrophysics; solar and stellar astrophysics; astrophysics of galaxies; Astrophysics and Astronomy; Physical Sciences and Mathematics; Stars, Interstellar Medium and the Galaxy
article description
We have performed a differential line-by-line chemical abundance analysis, ultimately relative to the Sun, of nine very metal-poor main-sequence (MS) halo stars, near [Fe/H] = -2 dex. Our abundances range from -2.66 ≤ [Fe/H] ≤ -1.40 dex with conservative uncertainties of 0.07 dex. We find an average [α/Fe] = 0.34 ±0.09 dex, typical of the Milky Way. While our spectroscopic atmosphere parameters provide good agreement with Hubble Space Telescope parallaxes, there is significant disagreement with temperature and gravity parameters indicated by observed colors and theoretical isochrones. Although a systematic underestimate of the stellar temperature by a few hundred degrees could explain this difference, it is not supported by current effective temperature studies and would create large uncertainties in the abundance determinations. Both 1D and hydrodynamical models combined with separate 1D non-LTE effects do not yet account for the atmospheres of real metal-poor MS stars, but a fully 3D non-LTE treatment may be able to explain the ionization imbalance found in this work.