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We present chemical abundance analyses of sodium, iron-peak andneutron-capture elements for 97 kinematically selected thick disk, inner haloand outer halo stars with metallicities -3.3<[Fe/H]<-0.5. The main aim of thisstudy is to examine chemical similarities and differences among metal-poorstars belonging to these old Galactic components as a clue to determine theirearly chemodynamical evolution. In our previous paper, we obtained abundancesof alpha elements by performing a one-dimensional LTE abundance analysis basedon the high-resolution (R~50000) spectra obtained with the Subaru/HDS. In thispaper, a similar analysis is performed to determine abundances of an additional17 elements. We show that, in metallicities below [Fe/H]~-2, the abundanceratios of many elements in the thick disk, inner halo, and outer halosubsamples are largely similar. In contrast, in higher metallicities([Fe/H]>-1.5), differences in some of the abundance ratios among the threesubsamples are identified. Specifically, the [Na/Fe], [Ni/Fe], [Cu/Fe], and[Zn/Fe] ratios in the inner and outer halo subsamples are found to be lowerthan those in the thick disk subsample. In contrast to what was observed for[Mg/Fe] in our previous paper, [Eu/Fe] ratios are more enhanced in the two halosubsamples rather than in the thick disk subsample. The observed distinctchemical abundances of some elements between the thick disk and inner/outerhalo subsamples with [Fe/H]>-1.5 support the hypothesis that these componentsformed through different mechanisms. In particular, our results favor thescenario that the inner and outer halo components formed through an assembly ofmultiple progenitor systems that experienced various degrees of chemicalenrichments, while the thick disk formed through rapid star formation with anefficient mixing of chemical elements.

Chemical abundances of the Milky Way thick disk and stellar halo II.: sodium, iron-peak and neutron-capture elements