the nuclei from straying far from the valley of $\beta$ stability. The He intershell in asymptotic giant branch (AGB) stars is the site of the s-process as well as of C production. C and heavy elements are brought to the surface of the AGB stars during the “third dredgeup”. Since the r-process produces very neutron-rich nuclei initially, the r-process reaches the neutron magic numbers with considerably fewer protons than the s-process, and, as a result, these two processes produce abundance peaks at different atomic weights. As a result, when the solar-system total abundances ([$t_{ss}$]{}) are separated into contributions from the s-process ([$s_{ss}$]{}) and the r-process ([$r_{ss}$]{}) (e.g., Käppeler, Beer, & Wisshak, 1989; Arlandini [et al.]{} 1999), some elements are mostly contributed by the r-process, such as Eu, and some by the s-process, such as Ba and La. Therefore Eu is commonly referred to as an “r-process element” and Ba and La as “s-process elements”. The \[Eu/Ba\] and the \[Eu/La\] values are used to estimate the ratio of r-process to s-process contributions to the heavy element abundances in a star, increasing as the r-process fraction increases. Despite the nomenclature, it is important to remember that all neutron-capture elements lighter than Z=84 