Thermalization of Neutrinos in a Neutron Star Merger Simulation

TL;DR

This paper investigates neutrino behavior in neutron star merger simulations, showing that thermalization assumptions are valid only in hot, dense regions, and emphasizing the importance of non-equilibrium neutrino distributions for accurate microphysics modeling.

Contribution

It provides a detailed analysis of neutrino distributions post-merger, highlighting where thermalization assumptions break down and the significance of non-equilibrium effects in microphysics.

Findings

Thermalized neutrinos are consistent with MC results in hot, dense regions.

Departures from thermal predictions are significant in moderately warm regions.

Energy-averaged thermal assumptions do not ensure accurate weak interaction rates.

Abstract

We study the neutrino distributions that arise in a simulation of a neutron star merger that uses a Monte Carlo (MC) neutrino transport scheme. In a snapshot taken 1 ms after merger, we calculate relevant observables to test when neutrinos behave like a thermalized gas, and when a free-streaming picture is more appropriate. We find that in hot, dense regions where neutrino-matter interactions are frequent, MC neutrino and antineutrino distributions are consistent with thermalized neutrinos. In moderately warm regions, where neither approximation is expected to hold, we find significant departures from the predictions of the thermalized-neutrino approximation, particularly for the (anti)neutrino average opacity and net rate of absorption per baryon, even when average energies appear approximately thermal. At lower temperatures, MC results approach the free-streaming limit. Our results demonstrate that energy-averaged agreement with thermalized-neutrino assumptions does not guarantee accurate weak interaction rates. Non-equilibrium aspects of the neutrino distribution are therefore crucial for neutrino-mediated microphysics such as composition evolution in the early post-merger phase.