Binary neutron star merger simulations with hot microscopic equations of state

TL;DR

This paper presents advanced binary neutron star merger simulations using new finite-temperature equations of state, analyzing their impact on stability, gravitational waves, matter distribution, and ejecta, and evaluating universal relations.

Contribution

Introduces a new set of finite-temperature equations of state for neutron star merger simulations and systematically studies their effects on postmerger phenomena.

Findings

Finite temperature and rotation have opposing effects on stellar stability.

Identified the most suitable equations of state for accurate modeling.

Analyzed gravitational-wave signals and matter ejecta properties.

Abstract

We perform binary neutron star merger simulations using a newly derived set of finite-temperature equations of state in the Brueckner-Hartree-Fock approach. We point out the important and opposite roles of finite temperature and rotation for stellar stability and systematically investigate the gravitational-wave properties, matter distribution, and ejecta properties in the postmerger phase for the different cases. The validity of several universal relations is also examined and the most suitable EOSs are identified.