The observation of gamma rays from the beta decay of 26Al provides direct evidence of ongoing nucleosynthesis in the galaxy. While the observed galactic distribution of 26Al points to massive stars as the main production sites, the underlying nuclear processes are uncertain. Sensitivity studies have found that two reactions contributing to the uncertainty of 26Al production in massive stars are the 25Mg(α,n)28Si and 26Mg(α,n)29Si reactions. These reactions influence 26Al production in stable and explosive C/Ne shell burning in massive stars. The 26Mg(α,n)29Si has also been found to have a direct influence on the isotopic ratio of 29Si/30Si found in pre-solar grains formed from supernova. Models of supernova nucleosynthesis have failed to reproduce this ratio. While previous measurements of these reactions have been made, reaction rates rely solely on statistical model calculations in energy ranges where experimental data is present and in good agreement. Below this energy range, the reaction rates are based on discrepant, unpublished thesis data. To resolve these issues, measurements of the 25,26Mg(α,n)28,29Si total cross sections were performed with a newly developed active target detector at The University of Notre Dame's Nuclear Science Lab.