Chemical Compositions of Field Red Horizontal Branch Stars

Details Chemical Compositions of Field Red Horizontal Branch Stars Chemical Compositions of Field Red Horizontal Branch Stars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715308a&link_type=abstract

American Astronomical Society, AAS Meeting #217, #153.08; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Field Red Horizontal Branch stars (RHBs) are alleged to be members of the thick disk of our Galaxy and are an important evolutionary link between horizontal and asymptotic giant branch evolution. They are easy to identify in globular clusters through their color-magnitude diagram positions. However, they are harder to identify as single stars in the general field; thus they have received lesser attention to date. In this study, we composed a large catalog of RHB candidates and performed the first large-sample high-resolution spectroscopic survey of these stars. We have obtained high resolution spectra of a number of candidate field RHBs. The high resolution spectra of these stars were taken with the 2.7m Harlan J. Smith Telescope and Tull 2Dcoude (R=60000) spectrometer at McDonald Observatory. We have derived the metallicities and relative abundance ratios for some of the alpha (Ca and Si) and neutron capture (La and Eu) elements along with the fundamental stellar parameters. We have also determined CNO abundances in order to gain insight into the evolutionary states of the candidates. In particular, we have investigated the 12C/13C ratio using the CN features present in the 8000-8040 A region, which we have also used to obtain the N abundances of the candidates. Plausible RHB stars, members of the thick disk, found in our study, can shed light into Galactic evolutionary models.
This project has benefitted from the financial support of NSF (AST-0908978), the Rex G. Baker endowment to the University of Texas Astronomy Dept., and The Scientific and Technological Research Council of Turkey (TUBITAK).

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