A New Code for Proto-Neutron Star Evolution

TL;DR

This paper introduces a new, fully relativistic, one-dimensional code for simulating proto-neutron star evolution, incorporating advanced neutrino transport methods, and predicts a neutron-rich neutrino-driven wind, differing from previous models.

Contribution

The paper presents a novel general relativistic, implicit code with multi-group neutrino transport that improves upon previous models by predicting neutron-rich winds due to better charged-current interaction treatment.

Findings

Neutrino emission timescales are consistent with prior results.

The code predicts neutron excess in the neutrino-driven wind.

Simple flux-limited diffusion approximations are accurate within 10% for luminosities.

Abstract

A new code for following the evolution and emissions of proto-neutron stars during the first minute of their lives is developed and tested. The code is one dimensional, fully implicit, and general relativistic. Multi-group, multi-flavor neutrino transport is incorporated that makes use of variable Eddington factors obtained from a formal solution of the static general relativistic Boltzmann equation with linearized scattering terms. The timescales of neutrino emission and spectral evolution obtained using the new code are broadly consistent with previous results. Unlike other recent calculations, however, the new code predicts that the neutrino-driven wind will be characterized, at least for part of its existence, by a neutron excess. This change, potentially consequential for nucleosynthesis in the wind, is due to an improved treatment of the charged-current interactions of electron flavored neutrinos and anti-neutrinos with nucleons. A comparison is also made between the results obtained using either variable Eddington factors or simple equilibrium flux-limited diffusion. The latter approximation, which has been frequently used in previous studies of proto-neutron star cooling, accurately describes the total neutrino luminosities (to within 10%) for most of the evolution, until the proto-neutron star becomes optically thin.