Production factors relative to solar abundances of the main elements from core-collapse SNe (dotted lines), and from both core-collapse and pair-instability SNe (solid lines). The blue thin lines are the results using the Population III star models by Woosley & Weaver (1995) and Heger & Woosley (2002). The red thick lines correspond to the production factors using the values from Woosley & Weaver (1995) and our study (shown in Fig. 8).
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