A surprising number of them have \[Eu/La\] too high to be consistent with [$s_{ss}$]{} (Figure 5). Since Eu is predominately produced in the r-process in the solar system, the r-process is an clear choice for the source of Eu in CS 31062-050. If the r-process contributes an appreciable amount to the heavy elements then we would expect relatively high abundances of elements mostly or only produced in the r-process. Unfortunately, we could only obtain uninteresting upper limits for elements in the third r-process peak such as Os and Ir. However, the limit for Th, an r-only element, is more interesting.

![Log $\epsilon$(Eu) vs. log $\epsilon$(La) for a sample of CH (squares) and non-CH stars (triangles) with \[Fe/H\]$<-2.0$. The lines represent an [$r_{ss}$]{} ratio (solid), [$s_{ss}$]{} ratio (dot-dash) and [$t_{ss}$]{} ratio (dashed) of La to Eu. The non-CH stars are identified by their adherence to the [$r_{ss}$]{} line and have a wide range of Eu (and C) abundances. The CH stars have a wide range of La/Eu ratios and large enhancements in both elements. ](f5.eps){width="3.0in"}

Thorium abundance?
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We found an 3$\sigma$ upper limit to the abundance of Th of log$\epsilon=-0.85$. What does this tell us about the possible contributions of 