Implication of the Steady State Equilibrium Condition for Electron-Positron Gas in the Neutrino-driven Wind from Proto-Neutron Star

TL;DR

This paper investigates the steady state equilibrium condition in the electron-positron gas of neutrino-driven winds from proto-neutron stars, estimating initial electron fractions and their implications for r-process nucleosynthesis.

Contribution

It introduces a simple method to estimate initial electron fractions based on the equilibrium condition in the wind.

Findings

The equilibrium condition can be used to estimate initial electron fractions.

The condition may be suitable for r-process nucleosynthesis.

Provides a simplified approach for modeling neutrino-driven winds.

Abstract

Based on the steady state equilibrium condition for neutron-proton-electron-positron gas in the neutrino-driven wind from protoneutron star, we estimate the initial electron fraction in the wind in a simple and effective way. We find that the condition in the wind might be propriate for the r-process nucleosynthesis.