supersolar.

We can understand this tilt toward heavier nuclei as the result of a high neutron-to-seed ratio (Gallino [et al.]{} 1998). Figure 4 shows the abundances in CS 31062-050 compared with the results of an s-process in a 1.5$M_{\odot}$ AGB star with \[Fe/H\]$=-2.3$. (R. Gallino, private communication).

![The abundance in CS 31062-050 (filled circles) compared with an s-process calculation for a metal-poor AGB star. The top panel shows \[X/Fe\], which highlights the rise in overabundances of the neutron-capture elements as Z increases. The middle panel shows log $\epsilon$ vs. Z, which shows that the metal-poor s-process model does a better job of fitting the data than scaled solar system abundance patterns, although Eu and Er are both underpredicted. The difference between the model and the data is shown in the bottom panel.](f4.eps){width="3.0in"}

The top panel of Figure 4 shows the steep rise in \[El/Fe\] as Z increases, which is matched much better by the metal-poor s-process than by [$s_{ss}$]{}, although Y and Pb are not simultaneously fit. However, the agreement with Pd, Sm, Tb, Dy and Ho is very encouraging and a marked improvement over Figure 3. The bias to heavier nuclei can also be quantified using the light s-process 