“…The reaction also acts as a secondary neutron source during the s process in low-mass asymptotic giant branch (AGB) stars during which roughly half the abundances of nuclides in the A=90-209 range are thought to be synthesized [2]. A variety of attempts to experimentally determine the rate for this reaction at the Gamow window corresponding to s process temperatures (T = 0.2-0.3 GK) have been made either through direct 22 Ne(α,n) 25 Mg measurements [e.g., [3][4][5][6] or indirectly via 26 Mg(γ,n) 25 Mg [7], 25 Mg(n,γ) 26 Mg [8], 26 Mg(γ,γ') 26 Mg [9], 26 Mg(p,p'γ) 26 Mg [10], and 22 Ne( 6 Li,d) 26 Mg reactions [11,12]. However, direct measurements have been hindered by the small cross section due to the Coulomb barrier and the resonances at E α < 830 keV have not been identified with this method.…”