2009/12/23 by Jiang Zhang, Wenyuan Cui, Bo Zhang · 31 citations
Physics and Astronomy · #Abundance (ecology) #Abundance of the chemical elements #Astronomy and Astrophysical Research #Chemical evolution #Giant star #Isotope #Metallicity #Nucleosynthesis #Scientific Research and Discoveries #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1111/j.1365-2966.2009.15947.x
published in Monthly Notices of the Royal Astronomical Society 402(2), 956-960 (Oxford University Press)
openalex publication_date 2009/12/23 · arxiv created 2010/10/22 · arxiv updated 2010/10/25 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The chemical abundances of metal-poor stars are excellent sources of information for setting new constraints on models of Galactic chemical evolution at low metallicities. In this paper we present an attempt to fit the elemental abundances observed in the bright, metal-poor giant HD 175305, and derive isotopic fractions using a parametric model. The observed abundances can be well matched by the combined contributions from s- and r-process material. The component coefficients of the r- and s-processes are C1= 3.220 and C3= 1.134, respectively. The Sm isotopic fraction in this star where the observed neutron-capture elements are produced is predicted to be f152+154= 0.582, which suggests that, even though the r-process is predominantly responsible for the synthesis of the neutron-capture elements in the early Galaxy, the onset of the s-process had already occurred at this metallicity of [Fe/H]=−1.6.