Fig. 8.
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Impact of the nuclear mass uncertainties obtained in Cases 1 to 4 on the mass fractions of stable nuclei (and long-lived Th and U) of the material ejected from the binary 1.38–1.38 M⊙ NSM model as a function of the atomic mass, A. Solar r-abundances (Goriely 1999) are shown in gray as a reference and are scaled to the peak value of the A = 130 abundance in the Case 1 simulation.
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