Speaker
Mr
Shiv Subedi
(Ohio University)
Description
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 use 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 preliminary simulation and sensitivity study 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 the Edwards Accelerator Lab at Ohio University.
Primary author
Mr
Shiv Subedi
(Ohio University)
Co-author
Dr
Zach Meisel
(Ohio University)