  We present the abundance analyses for the neutron-capture elements, and
discuss the observed abundance distributions in very metal-poor stars with
excesses of r-process elements. As has been found by previous abundance
studies, the star-to-star scatter in the abundances of neutron-capture elements
are very large. The abundance patterns of the heavy neutron-capture elements
(56 $\leq$ Z $\leq$ 70) in seven objects with moderate to large excesses of the
neutron-capture elements are similar to that of the solar system r-process
component. These results strongly suggest that the heavy neutron-capture
elements in these objects are primarily synthesized by the r-process. On the
other hand, the abundance ratios of the light neutron-capture elements (38
$\leq$ Z $\leq$ 46) exhibit a rather large dispersion. Our inspection of the
correlation between Sr and Ba abundances in very metal-poor stars reveals that
the dispersion of the Sr abundances clearly decreases with increasing Ba
abundance. This results support previous suggestions that the light
neutron-capture elements are likely to have been produced in different
astrophysical sites from those associated with the production of the heavier
ones. The Th/Eu abundance ratios (log(Th/Eu)) measured for the seven
r-process-enhanced stars range from -0.10 to -0.59. Since these very metal-poor
stars are believed to be formed in the early Galaxy, this result means that a
small dispersion appears in the abundance ratios between Th and rare-earth
elements, such as Eu, in very metal-poor stars. In order to apply the Th/Eu
ratios to estimates of stellar ages, further understanding for the Th
production by the r-process nucleosynthesis is required.
