Abundance Patterns Among Very Metal-Poor Stars in the Halo of the Galaxy: A Statistical Approach

Details Abundance Patterns Among Very Metal-Poor Stars in the Halo of the Galaxy: A Statistical Approach Abundance Patterns Among Very Metal-Poor Stars in the Halo of the Galaxy: A Statistical Approach

Apr 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010iaus..262..412p&link_type=abstract

Stellar Populations – Planning for the Next Decade, Proceedings of the International Astronomical Union, IAU Symposium, Volume 2

Astronomy and Astrophysics

Astronomy

Galaxy: Halo, Galaxy: Stellar Content, Stars: Abundances, Methods: Statistical

Scientific paper

The main goal of this work is to explore the abundance patterns of the very metal-poor stars ([Fe/H]<-2.0) observed by the HERES (Hamburg ESO R-process Enhanced Star - Christlieb et al. 2004) survey. This type of study allows the analysis of the correlations among chemical elements, and place some constraints on the operation of the neutron-capture (r and s) processes in the early Galaxy. This approach makes use of statistical tools, such as agglomerative nesting, which can identify the formation of natural groups based on relations among elemental abundances (e.g. [C/Fe], [Sr/Fe], [Ba/Fe], and [Eu/Fe]), and can also be used in a series of “large-sample like” studies.
This study provides a comprehensive analysis of a sample of 326 metal-poor stars, and introduces two new subclasses (r-0 and s-I) for metal-poor stars with determined abundances of neutron-capture elements, aiming to standardize the nomenclature for those objects and, by reproducing previous results, confirms the validity of the statistical method used.

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