We investigate the effects of triple-α and 12C(α, γ) 16O reaction rates on the production of supernova yields for a massive star of 25 MO. We combine the reaction rates to examine the rate dependence, where the rates are considered to cover the possible variation of the rates based on experiments on the earth and on theory. We adopt four combinations of the reaction rates from two triple-α reaction rates and two 12C(α, γ) 16O ones. First,we examine the evolution ofmassive stars of 20 MO and 25 MO whose helium cores correspond to helium stars of 6 MO and 8 MO, respectively. While the 25 MO stars evolve to the presupernova stages for all combinations of the reaction rates, the evolutionary paths of the 20 MO stars proceed significantly differently for some combinations, which are unacceptable for progenitors of supernovae. Second, we perform calculations of supernova explosions within the limitation of spherical symmetry and compare the calculated abundance ratios with solar system abundances. We can deduce some constraints to the reaction rates. The results show that a conventional rate is adequate for a triple-α reaction rate and a rather higher value of the reaction rate within the upper limit for the experimental uncertainties is favorable for a 12C(α, γ) 16O rate.
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