The Impact of Helium-Burning Reaction Rates on Massive Star Evolution and Nucleosynthesis

TL;DR

This study investigates how uncertainties in helium-burning reaction rates affect the evolution and nucleosynthesis yields of massive stars, highlighting the importance of precise reaction rate measurements for accurate stellar modeling.

Contribution

It provides a comprehensive analysis of the sensitivity of massive star evolution to helium-burning reaction rate variations, including detailed nucleosynthesis predictions and implications for supernova outcomes.

Findings

Production factors agree within +/-25% for reaction rate variations

s-only isotopes favor higher R_3a values

Small changes in reaction rates cause sharp shifts in stellar convection and yields

Abstract

We study the sensitivity of presupernova evolution and supernova nucleosynthesis yields of massive stars to variations of the helium-burning reaction rates within the range of their uncertainties. We use the current solar abundances from Lodders (2009) for the initial stellar composition. We compute a grid of 12 initial stellar masses and 176 models per stellar mass to explore the effects of independently varying the 12^C(a,g)16^O and 3a reaction rates, denoted R_a12 and R_3a, respectively. The production factors of both the intermediate-mass elements (A=16-40) and the s-only isotopes along the weak s-process path (70Ge, 76Se, 80Kr, 82Kr, 86Sr, and 87Sr) were found to be in reasonable agreement with predictions for variations of R_3a and R_a12 of +/-25%; the s-only isotopes, however, tend to favor higher values of R_3a than the intermediate-mass isotopes. The experimental uncertainty (one standard deviation) in R_3a(R_a12) is approximately +/-10%(+/-25%). The results show that a more accurate measurement of one of these rates would decrease the uncertainty in the other as inferred from the present calculations. We also observe sharp changes in production factors and standard deviations for small changes in the reaction rates, due to differences in the convection structure of the star. The compactness parameter was used to assess which models would likely explode as successful supernovae, and hence contribute explosive nucleosynthesis yields. We also provide the approximate remnant masses for each model and the carbon mass fractions at the end of core-helium burning as a key parameter for later evolution stage