Comparison of the ﹩\mathrm{log}\,\epsilon ( \mathrm{X}\,) ﹩ abundances for ﹩Z> 30﹩ in HD 221170 with the scaled solar r‐process predictions from Simmerer et al. (2004; solid red line) and those based on Arlandini* (largely 1999; with modifications as described in § 5.2; dotted blue line). Both sets of predictions have been normalized to the value derived for ﹩\mathrm{log}\,\epsilon ( \mathrm{Eu}\,) ﹩ in HD 221170. In the top panel, the upper limits and open circles with error bars denote the stellar abundances. The bottom panel displays the difference defined as ﹩\Delta \mathrm{log}\,\epsilon ( \mathrm{X}\,) \equiv \mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{pred}\,}-\mathrm{log}\,\epsilon ( \mathrm{X}\,) _{\mathrm{obs}\,}﹩, where the error bars are those we adopted for the abundances derived for each element. Upper limits are not displayed in the bottom panel.