Abstract
A very-massive star forming a massive CO core of \(\sim \)60–120 \(M_\odot \) is considered to explode as a pair-instability supernova (PISN). We have calculated the PISN nucleosynthesis taking both rotating and non-rotating progenitors for the first time to conduct a systematic comparison between theoretical yields and a large sample of metal-poor star abundances. We have found that the predicted low [Na/Mg] \(\sim \) -1.5 and high [Ca/Mg] \(\sim \) 0.5–1.3 abundance ratios are the most important to discriminate PISN signatures from normal metal-poor star abundances, and have confirmed that no currently observed metal-poor star matches with the PISN abundance. The confirmation of the non-detection may indicate that something important is missing from current understanding of stellar physics. Finally, we discuss that qualitatively different stellar evolution, which is against the PISN explosion, results from a CO core with a higher C fraction than canonical models.
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