Fig. 13.
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Gravitational neutron star mass MNS, grav as a function of the central specific entropy sc of the progenitor stars for Case A (panel a), Case B (panel b), and Case C (panel c) accretion. The dashed black line is the exponential fit to the neutron star masses of single stars computed for different convective boundary mixing found by Temaj et al. (2024).
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