CS 29497-034, and concluded that the observed abundances could not be fit by either a scaled solar-system s-process ([$s_{ss}$]{}) or scaled solar-system r-process ([$r_{ss}$]{}), but instead reflected enrichment by both processes.

A02 and Johnson & Bolte (2002a) also noted a large spread in \[Eu/Ba\] for other CH stars but suggested that the abundance pattern seen in these CH stars was due solely to the s-process, albeit one that produces a varying Eu/Ba ratio. A large percentage of CH stars have Eu/Ba ratios larger than [$s_{ss}$]{}. With the Hill [et al.]{} interpretation, this would suggest that a number of s-process-rich stars are also r-process rich. Some fraction of non-CH field stars are Eu-rich, so it would not be surprising to find some stars that began as r-process-rich and also were polluted by an AGB companion later in their lives. However, while seven of 32 non-CH stars in McWilliam [et al.]{} (1995) have \[Eu/Fe\][$\scriptscriptstyle \; \buildrel > \over \sim \;$]{}0.5, six of eight CH stars in A02 have such high Eu. So it appears that r-process enrichment cannot be the solution for [*all*]{} the high Eu CH stars (but see below).

Recently, Cohen [et al.]{} found an extreme example of non-[$s_{ss}$]{} ratios 