the r-process to the lighter neutron-capture elements, such as Eu? We cannot definitely predict the expected Eu abundance in CS 31062-050 from the Th abundance since the ratio between Eu and the initial Th value produced in the r-process is not always constant. One theoretical calculation predicts Th/Eu=0.496 (Cowan [et al.]{} 1999), and many stars show that to be a reasonable value (Sneden [et al.]{} 2000; Johnson & Bolte 2001; Cowan [et al.]{} 2002). While CS 31082-001 (Hill [et al.]{} 2002) clearly disagrees with this Th/Eu ratio, its implied Th/Eu$_{initial}$ is higher than the value we use here, which would only decrease the possible contribution to the r-process to the Eu abundance derived from our Th limit. If we use Th/Eu=0.496 and an age for CS 31062-050 of 14 Gyr, we find that at most 66% of our Eu abundance could come from the r-process. We can now perform the same calculation for the s-process contribution, using the observed La/Eu ratio and the solar system s-process ratio from Arlandini [et al.]{} (1999). Here we find that the s-process only contributes 23% of the Eu, leaving at least 10% of the Eu without a source. Either our assumed s-process or r-process 