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

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

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jphcs.202a2042s&link_type=abstract

Journal of Physics: Conference Series, Volume 202, Issue 1, pp. 012042 (2010).

Physics

Scientific paper

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. This 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, these two states have 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 "missing" 2+ state, respectively.

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