in the CH star HE 2148-1247. The measured Ba/Eu ratio was $\sim 100$ while theoretical calculations from Arlandini [et al.]{} (1999), for example, give Ba/Eu $\sim$ 640. They favored the addition of r-processed material as well as s-processed material to HE 2148-1247. Qian & Wasserburg [et al.]{} (2003), in a companion paper, proposed an intriguing theory for the creation of such “s+r”-process stars. First some s-processed material is accreted from the AGB companion, which turns into a white dwarf. Later in the evolution of the system, the white dwarf accretes matter from the polluted star and suffers an accretion-induced collapse (AIC) to a neutron star. The $\nu$-driven wind produces an r-process, which also pollutes the companion, but since the white dwarf lacks an H or He envelope, lighter elements, such as Fe, are not manufactured. Therefore, the remaining star is r-process [*and*]{} s-process-rich. The AIC could potentially deliver a strong kick to the neutron star, which could explain why some CH stars have recently been shown not to be members of binaries (Preston and Sneden 2001; Hill [et al.]{} 2000). Because the production of the s-process in the AGB star and the production of the r-process in the AIC are 