Abundance profiles of the s-nuclide ⁸⁸Sr (black) and the p-nuclide ⁷⁴Se (red) in the region of the star that is relevant for the p-process. The abundance profiles are shown at four different stages: at the birth of the star (or zero-age main-sequence, dotted lines), at the start of core oxygen burning (dash-dot lines, at this point, the ⁷⁴Se abundance is about zero, hence not visible on the plot), at the end of the hydrostatic post-processing calculation (dashed lines) and after the supernova explosion (solid lines).