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A small fraction (< 1%) of presolar SiC grains is suggested to have been formed  in the ejecta of classical novae. The 29P(p,γ)30S  reaction plays an important role in understanding the Si isotopic abundances in such  grains, 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,  and thus the nova nucleosynthetic path. The  29P(p,γ)30S reaction rate at nova temperatures is  determined by two low-lying 3+ and 2+ resonances above the proton  threshold at 4399 keV in 30S. Despite several experimental studies in the past,  however, only one of these two states has only been observed very recently. We have  studied the 30S nuclear structure via the 32S(p,t) 30S  reaction at 5 laboratory angles between 9° to 62°. We have observed 14 states, eleven of  which are above the proton threshold, including two levels at 4692.7 ± 4.5 keV and 4813.8  ± 3.4 keV that are candidates for the 3+ and the previously “issing”  2+ state, respectively

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