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

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1213..235s&link_type=abstract

FIFTH EUROPEAN SUMMER SCHOOL ON EXPERIMENTAL NUCLEAR ASTROPHYSICS. AIP Conference Proceedings, Volume 1213, pp. 235-238 (2010).

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Nucleosynthesis, Stellar Evolution, Novae, Nuclear Structure, Cosmic Ray Nucleosynthesis, Black Holes, Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Collective Levels

Scientific paper

A small fraction of presolar SiC grains is suggested to have been formed in the ejecta of classical novae. The Si isotopic abundances in such grains can be determined from the 29P(p,γ)30S reaction rate at nova temperatures. The Si isotopic abundances 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. 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 ``missing'' 2+ state, respectively.

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