Phys.Rev. C 104, L022802 (2021)

L.Canete, G.Lotay, G.Christian, D.T.Doherty, W.N.Catford, S.Hallam, D.Seweryniak, H.M.Albers, S.Almaraz-Calderon, E.A.Bennett, M.P.Carpenter, C.J.Chiara, J.P.Greene, C.R.Hoffman, R.V.F.Janssens, J.Jose, A.Kankainen, T.Lauritsen, A.Matta, M.Moukaddam, S.Ota, A.Saastamoinen, R.Wilkinson, S.Zhu

New constraints on the ²⁵Al (p, γ) reaction and its influence on the flux of cosmic γ rays from classical nova explosions

NUCLEAR REACTIONS ¹¹B(¹⁶O, p)²⁶Mg, E=19 MeV from Argonne ATLAS accelerator; measured Eγ, Iγ, γγ-coin, γ(θ) and level half-lives by DSAM using Gammasphere array of 99 HPGe detectors. ²H(²⁵Mg, p)²⁶Mg, E=10 MeV/nucleon from Texas A and M cyclotron; measured outgoing protons and scattered deuterons using the TIARA Si array, and ²⁶Mg recoils by the MDM-2 magnetic spectrometer with Oxford ionization chamber, angular distributions of scattered deuterons and protons. ²⁶Mg; deduced levels, J, π, resonances, spectroscopic factors. ²⁶Si; deduced levels, resonances, J, π, Γ_p, Γ_γ, resonance strengths by comparing with the level structures of mirror nucleus ²⁶Mg. ²⁵Al(p, γ)²⁶Si, T=0.2-0.4 GK; deduced stellar reaction rate by considering the contribution of resonant states in ²⁶Si, galactic abundance of ²⁶Al from classical novae; performed nova outburst simulations using the hydrodynamic Lagrangian time-implicit code SHIVA.

doi: 10.1103/PhysRevC.104.L022802