to heavy s-process ratio \[ls/hs\]. The value for CS 31062-050 (using the elements suggested by Busso [et al.]{}, 2001) is 1.39, in good agreement with predictions for the s-process in \[Fe/H\]$\sim -2.5$ AGB stars and with other observations of CH stars (Busso [et al.]{} 2001). This model predicts no appreciable production of Cu or Zn. The low Cu and Zn observed in CS 31062-050 (Table 2) are also consistent with the conclusions of Matteucci [et al.]{} (1993) that Cu is primarily made in either explosive nucleosynthesis or the weak s-process and Zn in explosive nucleosynthesis, because they are clearly not made in the AGB star that polluted CS 31062-050.

The most glaring misfits in the Z$\geq 56$ range are the abundances of Eu and Er (and, with larger error bars, Ba). It was a similar observation, in particular the high Eu abundance, that prompted the suggestions of Hill [et al.]{} and Cohen [et al.]{} (2003) that CH stars with this characteristic were rich in both the s- and r-process. We now examine this question in more detail.

Sources for the heavy elements in CS 31062-050
==============================================

There are now a number of very metal-poor CH stars with high-resolution abundance analyses. 