Level structure of the T z = − 1 nucleus Ar 34 and its relevance for nucleosynthesis in ONe novae

The $^{24}\mathrm{Mg}+^{12}\mathrm{C}$ fusion reaction was used to perform a detailed $\ensuremath{\gamma}$-ray spectroscopy study of the astrophysically important nucleus $^{34}\mathrm{Ar}$. In particular, an experimental setup, coupling the advanced $\ensuremath{\gamma}$-ray tracking array GRETINA with the well-established Argonne fragment mass analyzer (FMA), was employed to obtain excitation energies and spin-parity assignments for excited states in $^{34}\mathrm{Ar}$, both above and below the proton separation energy. For the first time, an angular distribution analysis of in-beam $\ensuremath{\gamma}$ rays from fusion-evaporation reactions, using a tracking array, has been performed and Coulomb energy differences of analog states in the $T=1,$ $A=34$ mirror system, explored from 0 to 6 MeV. Furthermore, we present a comprehensive discussion of the astrophysical $^{33}\mathrm{Cl}(p,\ensuremath{\gamma})$ stellar reaction rate, together with implications for the identification of nova presolar grains from sulfur isotopic abundances.