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

Recent observational advances have enabled high resolution mapping of $^{44}$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 $^{44}$Ti production in model calculations. We are using MESA (Modules for Experiments in Stellar Astrophysics) as a tool to investigate the previously identified sensitivities of $^{44}$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 the simulation results and 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 Edwards Accelerator Lab at Ohio University.