Abundances for HD 115444 (open squares), HD 186478 (crosses), HD 108577 (open triangles), and BD +8 2548 (filled circles). They have been scaled to match the Arlandini et al. (1999) solar system r‐process curve using the mean difference between the Sm, Eu, La, Ba, and Ce abundances. We also show the Käppeler et al. (1989) r‐process curve to illustrate the errors present in deriving solar system r‐process contributions. The differences between the two curves arise because of improved nuclear data and different physical conditions used during the s‐process. These s‐process predictions are then subtracted from the total solar system abundances to produce the curves shown here.