Physics – Nuclear Physics – Nuclear Theory
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004rpao.conf..138i&link_type=abstract
THE r-PROCESS The Astrophysical Origin of the Heavy Elements and Related Rare Isotope Accelerator Physics. Proceedings of the Fi
Physics
Nuclear Physics
Nuclear Theory
Scientific paper
Observed large star-to-star scatters in chemical abundances of metal-poor stars may indicate that the inter-stellar gas was not fully mixed at the early epoch of the Galactic evolution. We construct an inhomogeneous chemical evolution model, and compare predicted stellar abundance distributions with observations, using statistical method. We take several supernova yields; the data of Nomoto et al. (1997) and Woosley & Weaver (1995), and discuss consistency of these yield sets with observations. In particular, we discuss the origin of r-process, from the point of view of enrichment of europium. Using the Subaru HDS, we have estimated Eu abundances of three extremely metal-poor stars with [Fe/H] ≲ -3. Comparison with our Galactic evolution model implies the dominant source of Eu to be the low-mass end of the supernova mass range.
Aoki Wako
Ishimaru Yuhri
Prantzos Nikos
Ryan Sean G.
Wanajo Shin-ya
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