Spectroscopic factors for low-lyingN16levels and the astrophysicalN15(n,γ)N16reaction rate

Abstract

Background: Fluorine is a key element for nucleosynthetic studies since it is extremely sensitive to the physical conditions within stars. The astrophysical site to produce fluorine is suggested to be asymptotic giant branch stars. In these stars the N15(n,γ)N16 reaction could affect the abundance of fluorine by competing with N15(α,γ)F19. Purpose: The N15(n,γ)N16 reaction rate depends directly on the neutron spectroscopic factors of the low-lying states in N16. Shell model calculations and two previous measurements of the (d,p) reaction yielded the spectroscopic factors with a discrepancy by a factor of ∼2. The present work aims to explore these neutron spectroscopic factors through an independent transfer reaction and to determine the stellar rate of the N15(n,γ)N16 reaction. Methods: The angular distributions of the N15(Li7,Li6)N16 reaction populating the ground state and the first three excited states in N16 are measured using a Q3D magnetic spectrograph and are used to derive the spectroscopic factors of these states based on distorted wave Born approximation analysis. Results: The spectroscopic factors of these four states are extracted to be 0.96 ± 0.09, 0.69 ± 0.09, 0.84 ± 0.08, and 0.65 ± 0.08, respectively. Based on the new spectroscopic factors we derive the N15(n,γ)N16 reaction rate. Conclusions: The accuracy and precision of the spectroscopic factors are enhanced due to the first application of high-precision magnetic spectrograph for resolving the closely spaced N16 levels which cannot be achieved in most recent measurements. The present result demonstrates that two levels corresponding to neutron transfers to the 2s1/2 orbit in N16 are not good single-particle levels although N15 is a closed neutron-shell nucleus. This finding is contrary to the shell model expectation. The present work also provides an independent examination to shed some light on the existing discrepancies in the spectroscopic factors and the N15(n,γ)N16 rate.Received 21 November 2013DOI:https://doi.org/10.1103/PhysRevC.89.012801©2014 American Physical Society