Fig. 3.
Adopted models for pair-instability pulsation supernova mass loss. For a given He core mass we show the mass of a star after PPSN mass loss. Moderate PPSN mass loss is adopted directly from Leung et al. (2019), while its modified (50% reduced mass loss) version is presented as weak PPSN model. Strong PPSN are adopted from Belczynski et al. (2016c).
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