solar system. CS 22892-052 (Sneden [et al.]{} 1996, 2000), HD 115444 (Westin [et al.]{} 2000) and CS 31082-001 (Cayrel [et al.]{} 2001) are the best studied members of this class. Studies have showed a remarkable similarity in the abundance ratios for elements between Ba (Z$=56$) and Hf (Z$=72$), (c.f. Truran [et al.]{} 2002) although in the lighter and heavier r-process element peaks there is considerable star-to-star scatter in abundance ratios (e.g., Sneden [et al.]{} 2000; Johnson & Bolte 2002b; Hill [et al.]{} 2002). Some r-process-rich stars, in particular CS22892-052, are also C-rich. The source of that C is unknown. Finally, we note that very metal-poor stars with low \[neutron-capture/Fe\] ratios have abundance patterns between Ba and Hf that agree with [$r_{ss}$]{} (Sneden & Parthsarathy 1983; Gilroy [et al.]{} 1988; Johnson & Bolte 2001).

Some puzzles and challenges
---------------------------

As more detailed studies of very metal-poor CH stars became available, some stars and elements did not fit neatly into the picture described above. Despite having lower \[Eu/Ba\] than the r-process-element-rich stars, in some CH stars \[Eu/Ba\] is higher than that [$s_{ss}$]{} or than predicted for the metal-poor s-process. Hill [et al.]{} (2000) analyzed spectra of two CH stars, CS 22948-027 and 