What do Metal-Poor Stars Tell?:. Origin of O-Zn and R-Process Elements

Details What do Metal-Poor Stars Tell?:. Origin of O-Zn and R-Process Elements What do Metal-Poor Stars Tell?:. Origin of O-Zn and R-Process Elements

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005omeg.conf...92i&link_type=abstract

ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2003. Held 17-19 November 2003 in RIKEN, Wako, Saitama, Japan. Edited by M Terasawa,

Astronomy and Astrophysics

Astronomy

Scientific paper

Observed large dispersions in chemical abundances of metal-poor stars may indicate that the inter-stellar gas was not mixed enough at the early epoch. 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.

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