  The CH star CS 31062-050 ([Fe/H]=-2.42) is one of the most useful stars yet
discovered for evaluating the s-process in metal-poor stars. It is very
abundant in heavy elements (e.g., [La/Fe]=2.2), and its relatively cool
temperature and low gravity mean that there are many lines of interesting
elements present in the spectrum. We measured the abundances of 22 elements
with Z>29, including the rarely measured Lu and Pd. We derive an upper limit on
the Th abundance as well. The abundances in CS 31062-050 show a similar pattern
to many other metal-poor CH stars: high [Pb/Fe] and [Pb/La] ratios, low [Y/La]
ratios and high [Eu/La] values compared to the solar system s-process. However,
the Th limit, with additional assumptions, is not consistent with the idea that
the excess Eu in CS 31062-050 is contributed by the r-process. In addition, the
observed [Eu/Tb] cannot be explained by any ratio of solar-system s-process and
r-process abundances. We therefore argue that the abundance pattern in CS
31062-050 is most likely the result of the s-process, and we discuss possible
modifications that could explain the non-solar-system pattern observed.
