A new approximation for heavy-lepton neutrino pair processes in simulations of core-collapse supernovae

TL;DR

This paper introduces a new efficient approximation for heavy-lepton neutrino pair processes in supernova simulations, demonstrating its accuracy and exploring how different physical assumptions influence the neutrino signals and proto-neutron star evolution.

Contribution

The paper presents a novel approximation method for neutrino pair production that closely matches full treatments and assesses its impact across different equations of state in supernova models.

Findings

New approximation matches full treatment results well

Impact of modifications depends on the EOS used

Variations due to formalism are smaller than EOS effects

Abstract

In this paper, we present a new approximation for efficiently and effectively including heavy-lepton neutrino pair-production processes in neutrino transport simulations of core-collapse supernovae. In the neutrino-driven explosion mechanism, the electron neutrinos and anti-neutrinos are the main players in transporting the energy of the cooling PNS to the matter behind the shock. While heavy-lepton neutrinos, $\nu_x$, play a smaller role in the heating of the gain region, they dominate the cooling of the proto-neutron star (PNS) and therefore still play a crucial role in the explosion mechanism. In this study, we explore the impacts of modifications in the transport and formalisms of pair ($\nu_x\bar{\nu}_x$) emission and absorption processes. We quantify the impact in terms of the emergent neutrino signal and the nature of the PNS convection and early cooling. For this, we perform a set of simulations, spherically symmetric and axisymmetric, of a 20 M$_\odot$ progenitor using two different state-of-the-art equations of state (EOS). First and foremost, we show that our new efficient approximation for neutrino pair production matches the results of a full treatment very well. Furthermore, for this progenitor, we show that the impact of the modifications is dependent on the EOS used, as the EOS drives the PNS evolution. The variations we explore, including variations due to the nucleon-nucleon bremsstrahlung formalism, have a comparatively smaller impact than the EOS has as a whole.