Total Energy in Supernova Neutrinos and the Tidal Deformability and Binding Energy of Neutron Stars

TL;DR

This paper explores the relationship between supernova neutrino energy, neutron star binding energy, and tidal deformability, using gravitational wave data and equations of state to refine predictions and implications for supernova physics.

Contribution

It establishes a strong correlation between tidal deformability and neutron star binding energy, improving predictions of supernova neutrino energy and implications for new physics.

Findings

Minimum neutron star binding energy ~1.5×10^{53} ergs.

Neutrino energy below this suggests unobserved particles.

Neutrino energy above 6×10^{53} ergs indicates very massive neutron stars.

Abstract

The energy radiated in supernova neutrinos is a fundamental quantity that is closely related to the gravitational binding energy of a neutron star. Recently the tidal deformability of neutron stars was constrained by gravitational wave observations. By considering several equations of state, we find a strong correlation between the tidal deformability and neutron star binding energy. We use this correlation to sharpen predictions of the binding energy of neutron stars and the total neutrino energy in supernovae. We find a minimum binding energy for a neutron star formed in a supernova of $\sim1.5\times 10^{53}$ ergs. Should the neutrino energy in a supernova be significantly below this value, it would strongly suggest new unobserved particles are carrying away some of the supernova energy. Alternatively, if the neutrino energy is observed above $\sim 6\times 10^{53}$ ergs, it would strongly imply the formation of a (perhaps surprisingly) massive neutron star.