Mass-weighted nucleosynthesis yields at t ≃ 5 × 10⁴ s for the BLh (left column) and DD2 (right column) ejecta profiles. Top panels: Final yields for the simulations performed with in situ NN (blue) or using analytical fits for the nuclear power and post-processing the nucleosynthesis either on the original thermodynamic trajectories (orange), or on analytical density evolutions prescribed from a grid of initial thermodynamic conditions, with a standard (green) or double (red) resolution on the Y_e, τ, s grid. The black dots represent the Solar r-process abundances (Prantzos et al. 2020). All the abundances are scaled to produce a unitary total abundance of the elements with 170 ≤ A ≤ 200. The histogram shows, for the in situ NN run, the global cumulative mass fractions of the first (blue), second (orange) and third (purple) r-process peaks, and the rare-earths (brown). Bottom panel: relative differences against the simulation with in situ NN. The upward [downward] triangles indicate discrepancies greater than two orders of magnitude [smaller than 5 × 10⁻⁴]. The horizontal dashed lines highlight the 1% and factors of 1 and 10 discrepancies.