Metallicity Discrepancy between RGB and RHB Stars of the Globular Cluster M15

Details Metallicity Discrepancy between RGB and RHB Stars of the Globular Cluster M15 Metallicity Discrepancy between RGB and RHB Stars of the Globular Cluster M15

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc..990..184s&link_type=abstract

FIRST STARS III: First Stars II Conference. AIP Conference Proceedings, Volume 990, pp. 184-186 (2008).

Computer Science

Population Ii Stars, Globular Clusters In The Milky Way, Abundances, Chemical Composition, Origin, Formation, And Abundances Of The Elements, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Giant And Subgiant Stars

Scientific paper

The surveys of Sneden et al. (1997, 2000) found star-to-star abundance scatter of the light elements and the neutron-capture elements in M15 Red Giant Branch (RGB) stars. Further examination of three select RGB tip stars revealed a distinct r-process nucleosynthetic signature (consistent with a scaled solar system r-process abundance distribution). As part of a general survey of metal-poor red horizontal branch (RHB) stars, Preston et al. (2006) observed six RHB members of M15. They detected some star-to-star abundance scatter in both the light and n-capture elements. Notably, Preston et al. found that the mean metallicity of these stars was significant lower (by roughly 0.2 dex) than their RGB counterparts. We present a new comparative abundance derivation for three RGB and six RHB stars of the globular cluster M15. We make a considerable effort to understand the apparent discrepancy in the metallicity of RGB and RHB stars. We then perform a detailed examination of the n-capture elements. We will discuss the abundance results and consider the chemical inhomogeneity of M15.

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