Impact of Beta Decay on Antineutrino Spectra in Core-Collapse Supernovae

The role of weak interactions in core-collapse supernovae (CCSN) is critical to understanding both the dynamics of collapse and the neutrino-driven feedback that shapes the explosion. A key question is the relative contribution of different weak processes to (anti)neutrino emission in stellar cores. Prior research has focused on electron capture as the dominant weak process, though some studies suggest beta decay may compete under certain temperature and density conditions. To quantify this effect, we developed a high-performance pipeline using the NuLib neutrino interaction library to compute average (anti)neutrino energies and emissivities, which are then integrated into the GR1D supernova simulation code. Beta decay rates in hot stellar environments are calculated across the nuclide chart using a theoretical framework based on nuclear density functional theory (DFT) and finite-temperature quasiparticle random-phase approximation (FT-QRPA). These rates yield neutrino and antineutrino spectra, which are incorporated into GR1D to assess their impact on supernova evolution. In this presentation, I will show the resulting antineutrino spectra and discuss their implications. I will also outline future directions, including plans to extend the new spectra into 3D CCSN simulations.