Supernova Neutrino Light Curves and Spectra for Various Progenitor Stars: From Core Collapse to Proto-neutron Star Cooling

TL;DR

This paper provides detailed supernova neutrino light curves and spectra from simulations across various progenitor stars, aiding future detection efforts and theoretical background for supernova neutrino research.

Contribution

It introduces a comprehensive set of neutrino emission models for different progenitors, combining hydrodynamic and diffusion calculations to cover the entire supernova evolution.

Findings

Neutrino signals vary significantly with progenitor mass and metallicity.

The shock revival time influences neutrino emission characteristics.

Data is publicly available for broader research use.

Abstract

We present a new series of supernova neutrino light curves and spectra calculated by numerical simulations for a variety of progenitor stellar masses (13-50Msolar) and metallicities (Z = 0.02 and 0.004), which would be useful for a broad range of supernova neutrino studies, e.g., simulations of future neutrino burst detection by underground detectors, or theoretical predictions for the relic supernova neutrino background. To follow the evolution from the onset of collapse to 20 s after the core bounce, we combine the results of neutrino-radiation hydrodynamic simulations for the early phase and quasi-static evolutionary calculations of neutrino diffusion for the late phase, with different values of shock revival time as a parameter that should depend on the still unknown explosion mechanism. We here describe the calculation methods and basic results including the dependence on progenitor models and the shock revival time. The neutrino data are publicly available electronically.