New Determination of the 14C(n, γ)15C Reaction Rate and Its Astrophysical Implications

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Abstract We present a novel experiment to investigate the spectroscopic factor (SF) of the 15C ground state for the first time using single-neutron removal transfer reactions on 15C. Two consistent SFs were derived from the (p, d) and (d, t) reactions, which were subsequently used to deduce the 14C(n, γ)15C reaction cross section and the corresponding stellar reaction rate. A typical cross section of 3.89 ± 0.76 μb is determined at E c . m . = 23.3 keV. At the temperature range of 0.01–4 GK, our new reaction rate is 2.4–3.7 times higher than that of the first direct measurement and 20%–25% lower than that of the most recent direct measurement. Moreover, it is interesting that we can associate a long-standing nuclear structure issue, i.e., the so-called “quenching” effect, with this astrophysically relevant reaction. Finally, motivated by astrophysical interests of this reaction decades ago, implications of our new rate for several astrophysical problems are evaluated using state-of-the-art theoretical models. Our calculations demonstrate that the abundances of 14N and 15N can be enhanced in the inner regions of asymptotic giant branch stars, though with minimal impact on the chemical compositions of the interstellar medium. In the inhomogeneous Big Bang nucleosynthesis, the updated reaction rate can lead to a ∼20% variation in the final yields of 15N in neutron-rich regions. For the r-process in the core-collapse supernovae, a slight difference of ∼0.2% in the final abundances of heavy elements with A > 90 can be found by using our new rate.

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