Beta equilibrium in neutron star mergers
Nuclear Theory
2019-01-02 v2 High Energy Astrophysical Phenomena
High Energy Physics - Phenomenology
Abstract
We show that the commonly used criterion for beta equilibrium in neutrino-transparent dense nuclear matter becomes invalid as temperatures rise above 1 MeV. Such temperatures are attained in neutron star mergers. By numerically computing the relevant weak interaction rates we find that the correct criterion for beta equilibrium requires an isospin chemical potential that can be as large as 10-20 MeV, depending on the temperature at which neutrinos become trapped.
Cite
@article{arxiv.1803.00662,
title = {Beta equilibrium in neutron star mergers},
author = {Mark G. Alford and Steven P. Harris},
journal= {arXiv preprint arXiv:1803.00662},
year = {2019}
}
Comments
Section on neutrino mean free paths added. Discussion and plot of effect of isospin chemical potential on beta-equilibrium proton fraction added