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Observed large scatters in abundance ratios of neutron-capture elements relative to iron in metalpoor stars may suggest incomplete mixing of the interstellar medium at the beginning of the Galaxy. On the other hand, recent studies of metal-poor stars show considerable small dispersions for abundance ratios of C-Zn. We discuss whether such variations of scatters in abundance ratios can be explained by a consistent chemical evolution model. We also attempt to constrain the origins of r-process elements, comparing predictions by an inhomogeneous chemical evolution model with new observational results with SubaruHDS.

Chemical evolution of C-Zn and r-process elements produced by the first generation stars