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This study uses a modified potential cluster model to analyze two competing nuclear reactions involving carbon-14. The researchers calculated that proton capture overtakes neutron capture in producing nitrogen-15 at a transition temperature of 2.5 billion Kelvin, which is significantly higher than previous estimates. They also examined how deviations from thermal equilibrium affect this transition temperature.
Why it matters
These findings provide more accurate nuclear physics data for modeling stellar nucleosynthesis processes, particularly relevant for understanding element formation in stars and other astrophysical environments where carbon-14 reactions occur at extreme temperatures.
⚠️ Preprint – Noch nicht peer-reviewed
Dieser Artikel wurde noch nicht von unabhängigen Experten begutachtet. Die Ergebnisse sind vorläufig und sollten mit Vorsicht interpretiert werden.
Abstract: We present the first self-consistent theoretical study of the competing $^{14}mathrm{C}(n,gamma)^{15}mathrm{C}$ and $^{14}mathrm{C}(p,gamma)^{15}mathrm{N}$ reactions within the same modified potential cluster model (MPCM). For the $^{14}$C$(p,gamma_{0})^{15}$N reaction, total cross sections, astrophysical $S$ factors, and reaction rates are calculated using interaction potentials constrained by the available scattering and bound-state data. The astrophysical $S$-factor is estimated as $S(0)=4.5(1)$~keV$cdot text{b}$. Combining these results with our recent MPCM calculations for $^{14}mathrm{C}(n,gamma)^{15}mathrm{C}$, we determine the transition temperature at which proton capture overtakes neutron capture in the production of $^{15}mathrm{N}$. The self-consistent comparison predicts a transition temperature $T_9^{rm c.p.}=2.5$ under Maxwell–Boltzmann statistics, significantly higher than previous estimates. The analysis is extended to Tsallis statistics, demonstrating that deviations from thermal equilibrium produce substantial shifts of the transition temperature. These results provide improved nuclear-physics input for astrophysical nucleosynthesis calculations.