Comprehensive neutrino light curves and spectra: from pre-supernova evolution to early supernova phase

Abstract

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~$M_\odot$. Our systematic analysis reveals that the compactness parameter ($ξ_{2.5}$) and carbon-oxygen core mass ($M_{\text{CO}}$) exhibit strong correlations with neutrino emission. In the pre-supernova phase, the time-integrated number of neutrinos correlates with $ξ_{2.5}$ when integrated over the final day and with $M_{\text{CO}}$ for longer durations. For the early supernova phase ($<200$ ms post-bounce), 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.

Figures (27)

• Figure 1: Method outline in this paper.
• Figure 2: Radial profiles of density, temperature, electron fraction, and electron chemical potential from top to bottom. We show six profiles at $t_{pb}\sim -10^6$ s, $-10^3$ s, $-1$ s, $-0.1$ s, 50 ms and 200 ms. Colors distinguish the progenitor models.
• Figure 3: Time evolution of number luminosities (left) and average energies (right) of $\nu_e$, $\bar{\nu}_e$ and $\nu_x$ from top to bottom. Colors distinguish the progenitor models.
• Figure 4: Neutrino spectrum for $\nu_e$, $\bar{\nu}_e$ and $\nu_x$ from top to bottom. We show six profiles at $t_{pb}\sim -10^6$ s, $-10^3$ s, $-1$ s, $-0.1$ s, 50 ms and 200 ms. Colors distinguish the progenitor models.
• Figure 5: Radial profiles of neutrino number densities for $\nu_e$ (top), $\bar{\nu}_e$ (middle) and $\nu_x$ (bottom) in preSN phase. We show the profiles at $t_{pb}\sim -10^6$, $-10^3$, $-1$ and $-0.1$ s from left to right. Colors distinguish the progenitor models.