Level structure of the <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msub><mml:mi>T</mml:mi><mml:mi>z</mml:mi></mml:msub><mml:mo>=</mml:mo><mml:mo>−</mml:mo><mml:mn>1</mml:mn></mml:mrow></mml:math> nucleus <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi>Ar</mml:mi><mml:mprescripts /><mml:none /><mml:mn>34</mml:mn></mml:mmultiscripts></mml:math> 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 advanced tracking array GRETINA with well-established Argonne fragment mass analyzer (FMA), employed obtain excitation energies and spin-parity assignments for excited states in $^{34}\mathrm{Ar}$, both above below proton separation energy. For first time, angular distribution analysis in-beam $\ensuremath{\gamma}$ rays from fusion-evaporation reactions, using array, has been performed Coulomb energy differences analog $T=1,$ $A=34$ mirror system, explored 0 6 MeV. Furthermore, we present comprehensive discussion astrophysical $^{33}\mathrm{Cl}(p,\ensuremath{\gamma})$ stellar rate, together implications identification nova presolar grains sulfur isotopic abundances.