of CH stars are often referred to as barium stars) and subsolar \[Eu/Ba\].

Theory predicts that s-process nucleosynthesis will depend on the initial metallicity of the AGB star and on its mass (Gallino [et al.]{} 1998; Goriely & Mowlavi 2000; Busso [et al.]{} 2001). Busso [et al.]{} reported s-process yields as a function of initial \[Fe/H\] and for AGB stars with 1.5 and 3.0M$_\odot$ and made comparisons with the available observational data. The basic metallicity dependence is a tilting of the s-process products toward heavier elements with decreasing \[Fe/H\] of the host AGB star. The prediction that $^{208}$Pb will have a particularly strong excess has been verified for CS 22183-015 (Johnson & Bolte 2002a), HE 0024-2523 (Lucatello [et al.]{} 2003) and many of the stars studied by Van Eck [et al.]{} (2001, 2003) and Aoki [et al.]{} (2002) (A02). On the other hand, Aoki [et al.]{}(2000, 2001) present the analysis of two metal-poor, s-process-rich stars, LP 625-44 and LP 706-7, which have \[Pb/Ba\] $\sim$ 0.

Very metal-poor r-process-rich stars
------------------------------------

There is a second class of neutron-capture-rich very metal-poor stars in which the abundance pattern of the heavy elements more closely follows that inferred for the r-process elements in the 