Nuclear Statistical Equilibrium neutrino spectrum

TL;DR

This paper investigates neutrino spectra emitted from plasma in nuclear statistical equilibrium, focusing on high-energy neutrinos, and introduces a new numerical method to analyze their production in astrophysical environments.

Contribution

A novel numerical approach for calculating nuclear abundances in NSE and analysis of neutrino spectra under various astrophysical conditions.

Findings

Identification of conditions favoring high-energy neutrino emission.

Analysis of Y_e values affecting neutrino production.

Results relevant for supernovae and neutron star mergers.

Abstract

The spectral emission of neutrinos from a plasma in nuclear statistical equilibrium (NSE) is investigated. Particular attention is paid to the possible emission of high energy (>10 MeV) neutrinos or antineutrinos. A newly developed numerical approach for describing the abundances of nuclei in NSE is presented. Neutrino emission spectra, resulting from general Fuller, Fowler, Newman (FFN) conditions, are analyzed. Regions of T-rho-Ye space favoring detectability are selected. The importance of critical Y_e values with zero net rate of neutronization (Ye dot) is discussed. Results are provided for the processing of matter under conditions typical for thermonuclear and core-collapse supernovae, pre-supernova stars, and neutron star mergers.