Phys.Rev. C 102, 035803 (2020)

A.Meyer, N.de Sereville, A.M.Laird, F.Hammache, R.Longland, T.Lawson, M.Pignatari, L.Audouin, D.Beaumel, S.Fortier, J.Kiener, A.Lefebvre-Schuhl, M.G.Pellegriti, M.Stanoiu, V.Tatischeff

Evaluation of the ¹³N(α, p)¹⁶O thermonuclear reaction rate and its impact on the isotopic composition of supernova grains

NUCLEAR REACTIONS ¹³C(⁷Li, t)¹⁷O^*, E=34 MeV; measured E(t), I(t), σ(θ) using Enge Split-Pole magnetic spectrometer at the Tandem-ALTO facility in Orsay. ¹⁷O; deduced levels, resonances, J, π, L-transfers from analysis of angular distributions with finite-range distorted wave Born approximation (DWBA) calculations, Γ_α, α-spectroscopic factors, and compared with previous experimental data, and evaluated data in the ENSDF database. ¹⁷O, ¹⁷F; comparison of levels resonances, spin-parities, and resonance parameters in mirror nuclei. ¹³N(α, p)¹⁶O, E(cm)=0.05-3.0 MeV; deduced astrophysical S-factor by R-matrix calculations using AZURE2 code, Monte-Carlo reaction rates from 0.01-10 GK, isotopic abundances in the He-shell ejecta of a supernova model, production factors of stable isotopes, in the mass region between ¹²C and ⁵⁰V.

doi: 10.1103/PhysRevC.102.035803