We used the Al(He,t)Si*(p)Al reaction at the Wright Nuclear Structure Laboratory to probe resonances of Al + p and Al + p for excitation energies of astrophysical interest. We used a beam of 25-MeV He ions produced by the ESTU Tandem at WNSL, and a target of 125 g/cm Al. Ejected tritons were detected at 0◦ in the gas ionization detector at the focal plane of the Enge Split-pole Spectrometer. Decay protons were detected in two position-sensitive silicon-strip detectors, located in the target chamber very close to the target, spanning an angular range of 55 − 125◦. We detected protons from the decay of states in Si as little as 600 keV above the proton threshold, populating the ground and first (metastable) and second excited states of Al. The excitation energies of states in Si that are resonances for Al + p and Al + p were determined. Work is ongoing to determine branching ratios for these decays, as well as resonance strengths, reaction rates, and consequences for stellar nucleosynthesis. The observation of Al in the galaxy [1] provided the first direct evidence for ongoing stellar nucleosynthesis. The gamma ray from the decay of Al is an observable that can be used to test astrophysical models of such nucleosynthesis sites as novae. These models use nuclear reaction rates as input. In order for the predictions made by the models to be reliable, the nuclear physics input also needs to be reliable: relevant reaction rates must be known to at least 20%. The Al(p,γ)Si reaction is important to the total amount of Al present in a star, since it is the only destruction mechanism of Al that competes with beta decay, thus preventing emission of the signature 1.8-MeV gamma ray. The rate is currently known to only about a factor of four. In addition to proton capture on the ground state, there could be proton captures on the low-energy metastable first excited state of Al. (Because this state has a very different spin from the ground state (0+ vs 5+), there is no direct communication between the two states, although at very high temperatures they can communicate via higher-lying states of intermediate spin; the states must therefore be treated as separate entities in most calculations.) No experimental information currently exists on Al(p,γ)Si. Any resonant contributions to this reaction rate could have a significant effect on the amount of Al synthesized in high-temperature astrophysical events.
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