Developing an end-to-end simulation framework of supernova neutrino detection

TL;DR

This paper presents an integrated, long-duration supernova neutrino simulation framework that models core-collapse to neutrino detection, aiding future observations and analysis of galactic supernovae.

Contribution

It introduces a new one-dimensional supernova simulation that runs for 20 seconds, providing detailed neutrino emission data for detection predictions.

Findings

Simulated 20-second neutrino emission from supernovae

Estimated 1,800 neutrino events in Super-Kamiokande for a supernova at 10 kpc

Compared simulation results with SN 1987A observations for validation

Abstract

Massive stars can explode as supernovae at the end of their life cycle, releasing neutrinos whose total energy reaches $10^{53}$ erg. Moreover, neutrinos play key roles in supernovae, heating and reviving the shock wave as well as cooling the resulting protoneutron star. Therefore, neutrino detectors are waiting to observe the next galactic supernova and several theoretical simulations of supernova neutrinos are underway. While these simulation concentrate mainly on only the first one second after the supernova bounce, the only observation of a supernova with neutrinos, SN 1987A, revealed that neutrino emission lasts for more than 10 seconds. For this reason, long-time simulation and analysis tools are needed to compare theories with the next observation. Our study is to develop an integrated supernova analysis framework to prepare an analysis pipeline for treating galactic supernovae observations in the near future. This framework deals with the core-collapse, bounce and proto-neutron star cooling processes, as well as with neutrino detection on earth in a consistent manner. We have developed a new long-time supernova simulation in one dimension that explodes successfully and computes the neutrino emission for up to 20 seconds. Using this model we estimate the resulting neutrino signal in the Super-Kamiokande detector to be about 1,800 events for an explosion at 10 kpc and discuss its implications in this paper. We compare this result with the SN 1987A observation to test its reliability.