Study of astrophysically important resonant states in 30S using the 32S(p,t)30S reaction

Abstract The 29 P(p, γ ) 30 S reaction plays an important role in understanding the Si isotopic abundances in presolar grains of nova origin, which in turn provide us with information on the nature of the probable white dwarf progenitor's core, as well as the peak temperatures achieved during nova outbursts. This rate at nova temperatures is determined by two low-lying 3 + and 2 + resonances above the proton threshold at 4399 keV in 30 S. We have studied the 30 S nuclear structure via the 32 S(p,t) 30 S reaction at 5 laboratory angles between 9 ° to 62 ° . We have observed 14 states including two levels at 4692.7 ± 4.5 keV and 4813.8 ± 3.4 keV that are candidates for the 3 + and the previously “missing” 2 + state, respectively.