Investigating and reducing the impact of nuclear reaction rate uncertainties on $ce{^{44}Ti}$ production in core-collapse supernovae

Recent observational advances have enabled high resolution mapping of $ce{^{44}Ti}$ in core-collapse supernova (CCSN) remnants. Comparisons between observations and 3D models provide stringent constraints on the CCSN mechanism. However, recent work has identified several uncertain nuclear reaction rates that influence $ce{^{44}Ti}$ production in model calculations. We use MESA (Modules for Experiments in Stellar Astrophysics) as a tool to investigate the previously identified sensitivities of $ce{^{44}Ti}$ production in CCSN to varied reaction rates. MESA is a code for modeling stellar evolution and stellar explosions in one-dimension. We will present our preliminary results of CCSN simulations and sensitivity study and will also discuss our plans to reduce or remove the most significant uncertainties from ($\alpha$, n), ($\alpha$, p), ($\alpha$, $\gamma$), (p, n) and (p, $\gamma$) reaction rates using direct and indirect measurement techniques at the Edwards Accelerator Lab at Ohio University.