Total gamma-ray yield from the reaction 45Sc (p,γ) 46Ti

This work describes a study of the nuclear reaction 45Sc(p, γ) 46Ti, a reaction of importance to calculations of nuclear abundances in supernova stars. The cross-section for this reaction was measured over the proton energy range 0.7 MeV to 4.2 MeV, to an accuracy of better than 20%. The experimental data and the predictions of the Hauser-Feshbach statistical model were used to calculate reaction rates in the stellar interior over the temperature range 109 to 1010 K