METAL-POOR STARS OBSERVED WITH THE MAGELLAN TELESCOPE. I. CONSTRAINTS ON PROGENITOR MASS AND METALLICITY OF AGB STARS UNDERGOING s-PROCESS NUCLEOSYNTHESIS
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Frebel_Metal-poor stars.pdf
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Author(s)
Placco, Vinicius M.
Beers, Timothy C.
Karakas, Amanda I.
Kennedy, Catherine R.
Rossi, Silvia
Christlieb, N.
Stancliffe, Richard J.
Frebel, Anna L.
Date Issued
May 2013
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Placco, Vinicius M., Anna Frebel, Timothy C. Beers, Amanda I. Karakas, Catherine R. Kennedy, Silvia Rossi, Norbert Christlieb, and Richard J. Stancliffe. “METAL-POOR STARS OBSERVED WITH THE MAGELLAN TELESCOPE. I. CONSTRAINTS ON PROGENITOR MASS AND METALLICITY OF AGB STARS UNDERGOING s-PROCESS NUCLEOSYNTHESIS.” The Astrophysical Journal 770, no. 2 (June 20, 2013): 104.
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Author's final manuscript
Abstract
We present a comprehensive abundance analysis of two newly discovered carbon-enhanced metal-poor (CEMP) stars. HE 2138?3336 is a s-process-rich star with [Fe/H] = -2.79, and has the highest [Pb/Fe] abundance ratio measured thus far, if non-local thermodynamic equilibrium corrections are included ([Pb/Fe] = +3.84). HE 2258?6358, with [Fe/H] = -2.67, exhibits enrichments in both s- and r-process elements. These stars were selected from a sample of candidate metal-poor stars from the Hamburg/ESO objective-prism survey, and followed up with medium-resolution (R ~ 2000) spectroscopy with GEMINI/GMOS. We report here on derived abundances (or limits) for a total of 34 elements in each star, based on high-resolution (R ~ 30, 000) spectroscopy obtained with Magellan-Clay/MIKE. Our results are compared to predictions from new theoretical asymptotic giant branch (AGB) nucleosynthesis models of 1.3? M [subscript ?] with [Fe/H] = ?2.5 and ?2.8, as well as to a set of AGB models of 1.0 to 6.0?M [subscript ?] at [Fe/H] = ?2.3. The agreement with the model predictions suggests that the neutron-capture material in HE 2138?3336 originated from mass transfer from a binary companion star that previously went through the AGB phase, whereas for HE 2258?6358, an additional process has to be taken into account to explain its abundance pattern. We find that a narrow range of progenitor masses (1.0 ? M(M [subscript ?]) ? 1.3) and metallicities (?2.8 ? [Fe/H] ??2.5) yield the best agreement with our observed elemental abundance patterns.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
http://dx.doi.org/10.1088/0004-637x/770/2/104
