Thermonuclear reaction rate of 30 Si($p, γ$) 31 P
Silicon synthesis in high-temperature hydrogen burning environments presents one possible avenue for the study of abundance anomalies in globular clusters. This was suggested in a prior study, which found that the large uncertainties associated with the Si 30 ( p , γ ) P 31 reaction rate preclude a firm understanding of the stellar conditions that give rise to the Mg-K anticorrelation observed in the globular cluster NGC 2419. In an effort to improve the reaction rate, we present new strength measurements of the E r lab = 435 keV and E r lab = 501 keV resonances in Si 30 ( p , γ ) P 31 . For the former, which was previously unobserved, we obtain a resonance strength of ω γ = ( 1.14 ± 0.25 ) × 10 – 4 eV. For the latter, we obtain a value of ω γ = ( 1.88 ± 0.14 ) × 10 – 1 eV, which has a smaller uncertainty compared to previously measured strengths. Based on these results, the thermonuclear reaction rate has been re-evaluated. The impact of the new measurements is to lower the reaction rate by a factor of ≈ 10 at temperatures important to the study of NGC 2419. The rate uncertainty at these temperatures has also been reduced significantly.