Comprehensive Neutrino Light Curves and Spectra: From Presupernova Evolution to Early Supernova Phase

We present the first systematic study of neutrino emissions from massive stars, continuously tracking the late evolutionary stages through the early core-collapse supernova phase. Using progenitor and supernova models, we analyze the neutrino luminosities and spectra for progenitors with initial masses of 10–40 M ⊙ . Our systematic analysis reveals that the compactness parameter ( ξ 2.5 ) and carbon–oxygen core mass ( M CO ) exhibit strong correlations with neutrino emission. In the presupernova phase, the time-integrated number of neutrinos correlates with ξ 2.5 when integrated over the final day and with M CO for longer durations. For the early supernova phase (<200 ms postbounce), the neutrino properties are relatively insensitive to the specific stellar evolution code used, allowing for a reliable extraction of physical correlations. We confirm that the neutrino emission features, including the electron neutrino burst properties and accretion-powered luminosity of other species, reflect the progenitor’s compactness. An evaluation of the observational feasibility for a nearby progenitor using a false-alarm-rate approach suggests that these correlations can persist even under practical detection conditions. Such a joint analysis of both phases provides complementary constraints on the internal structure. All calculated time-series data will be made publicly available.