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Fluorine is a key element for nucleosynthetic studies since it is extremelysensitive to the physical conditions within stars. The astrophysical site toproduce fluorine is suggested to be asymptotic giant branch (AGB) stars. Inthese stars the 15N(n, g)16N reaction could affect the abundance of fluorine bycompeting with 15N(a, g)19F. The 15N(n, g)16N reaction rate depends directly onthe neutron spectroscopic factors of the low-lying states in 16N. The angulardistributions of the 15N(7Li, 6Li)16N reaction populating the ground state andthe first three excited states in 16N are measured using a Q3D magneticspectrograph and are used to derive the spectroscopic factors of these statesbased on distorted wave Born approximation (DWBA) analysis. The spectroscopicfactors 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 factorswe derive the 15N(n,g)16N reaction rate. The accuracy and precision of thespectroscopic factors are enhanced due to the first application ofhigh-precision magnetic spectrograph for resolving the closely-spaced 16Nlevels which can not be achieved in most recent measurement. The present resultdemonstrates that two levels corresponding to neutron transfers to the 2s1/2orbit in 16N are not so good single-particle levels although 15N is a closedneutron-shell nucleus. This finding is contrary to the shell model expectation.The present work also provides an independent examination to shed some light onthe existing discrepancies in the spectroscopic factors and the 15N(n, g)16Nrate.

Spectroscopic factors for low-lying 16N levels and the astrophysical 15N(n,gamma)16N reaction rate