Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21542512f&link_type=abstract
American Astronomical Society, AAS Meeting #215, #425.12; Bulletin of the American Astronomical Society, Vol. 42, p.338
Astronomy and Astrophysics
Astronomy
Scientific paper
Horizontal branch (HB) stars are evolved helium core-burning objects that are observable as globular cluster members and halo field population. Those found in Galactic globular clusters exhibit various distributions of photometric colors (or temperatures), popularly called the "HB morphology". These distributions usually are subdivided into three groups: the stable bluer and redder portions of the HB, and the variable RR Lyrae stars in between. The practical assignment of star to a particular group is based on color (or temperature). However, the physical cause that determines the position of cluster HB stars can be due to multiple parameters (e.g. metallicity and age). We have conducted a detailed abundance ratios study of field HB stars (Teff< 9000K) to give potential insight into HB morphology from a different prespective.Here we present the preliminary results of the study. Such a controlled-sample and internally consistent analysis of many elements has never been previously conducted. Our analysis shows that the abundance ratios of almost all elements are consistent across 4000K domain for the first time. We will discuss any abundances anomalies and the implications on the HB evolution. This work is supported by NSF grant AST-0607708, AST-0908978 and Sigma Xi grants in aid.
Behr Bradford Bartholomew
For Bi-Qing
Sneden Chistopher
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