Speaker
Description
Recent advancements in neutrino detection technology, such as the gadolinium enhancement in Super-Kamiokande (SK-Gd), upgraded KamLAND, and upcoming mega-detectors like JUNO, Hyper-Kamiokande, and DUNE, have revolutionized our observational capabilities. These upgrades make it increasingly realistic to detect not only the neutrino during a core-collapse supernova but also the "pre-supernova" neutrinos emitted in the hours or days leading up to the explosion. Capitalizing on these technological breakthroughs, we present the first systematic study of neutrino emission from massive stars, continuously covering late evolutionary stages through the early core-collapse supernova phase. Using various progenitor and supernova models, we analyzed the neutrino luminosities and spectra for progenitor stars with initial masses of 10–40 $M_\odot$. Our systematic analysis reveals that neutrino emission characteristics strongly correlate with the progenitor's compactness parameter ($\xi_{2.5}$) and carbon-oxygen core mass ($M_{\text{CO}}$). In the pre-supernova phase, the time-integrated number of neutrinos correlates with $\xi_{2.5}$ over the final day before collapse, and with $M_{\text{CO}}$ over longer durations. Furthermore, during the early supernova phase (less than 200 ms post-bounce), neutrino properties—such as electron neutrino burst features and accretion-powered luminosity—are relatively insensitive to the specific stellar evolution code used. This robustness allows for a reliable extraction of physical correlations, confirming that neutrino emissions directly reflect the progenitor's compactness. Finally, we evaluated the observational feasibility for a nearby progenitor using a False Alarm Rate approach. Crucially, we demonstrate that even under realistic detection conditions, the correlation between the total number of detected neutrinos and $\xi_{2.5}$ remains clearly observable. Our findings suggest that future neutrino observations have the profound potential to directly constrain the internal structure of progenitor stars. All calculated time-series data will be made publicly available.