Analysis of the Astrophysically Important $^{28}$Si($p,t$)$^{26}$Si Reaction

Study of $^{26}$Al in astrophysical environments is important to models of Galactic chemical evolution because the observation of this long-lived radioactive nucleus in the Galaxy indicates that stellar nucleosynthesis has occurred ``recently'' (in the last million years). However, the source of $^{26}$Al production in nature is still an open question, in large part due to uncertainties in the $^{25}$Al($p,\gamma$)$^{26}$Si reaction rate arising from a lack of information on the $^{26}$Si level structure above the proton threshold. To rectify this, the $^{26}$Si level structure was measured at the Holifield Radioactive Ion Beam Facility through study of the $^{28}$Si($p,t$)$^{26}$Si reaction. A 40 MeV proton beam was used to bombard a natural Si target, and the energy and angular distibutions of tritons were measured to reveal important $^{26}$Si level information. Details of the data analysis will be presented.