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    Measurement of high-energy resonances in Ne22 through inverse kinematics

    B. Greaves1,2, D. Mücher3, S. Gillespie4,5, T. Drake6, L. Atar1, A. Babu4,7, F. Barrett4,8, N. Bernier4,9,10, S. S. Bhattacharjee4 et al.

    V. Bildstein1, R. Caballero-Folch4, W. N. Catford11, A. Chester5, C. Aa. Diget12,4, A. Garnsworthy4, G. Hackman4,13, E. Kasanda1,14, A. M. Laird12,4, B. Olaizola4,15, N. A. Orr16, T. Rockman1, Y. Saito4,9, P. Šiurytė17, A. Spyrou5,18, C. E. Svensson1,4, and R. Umashankar4,9

    Phys. Rev. C 113, 065806 – Published 17 June, 2026

    DOI: https://doi.org/10.1103/h5h1-xrj2

    Abstract

    The Ne22(α,n)Mg25 reaction acts as an s-process neutron source in both the main and weak s processes. By exciting Ne22 to highly energetic resonance states above 9.7 MeV, we measured the properties of these difficult-to-access states, which are relevant to the stellar production of this seed isotope through the O18(α,γ)Ne22 reaction. At the ISAC II facility of TRIUMF, a 165 MeV beam of Ne21 was delivered to a deuterated polyethylene (CD2) target, resulting in the population of an excited Ne22 nucleus and a recoil proton. This reaction mechanism was studied with two surrounding complementary arrays: SHARC, a segmented silicon array for measurement of recoil particles, and TIGRESS, a high-purity, segmented germanium clover array for measurement and correction of Doppler-shifted γ rays. Here, we present the first definitive spin-parity assignment and energy constraint of the 217 keV O18(α,γ)Ne22 resonance state, as well as the spin confirmation of the 575 keV and 662.1 keV resonances, and discuss the implications of these spin constraints on the production of the Ne22 isotope in asymptotic giant branch stars.

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