# Neutron-Star-Merger Equation of State

## TL;DR

This paper develops a comprehensive equation of state for neutron star matter, incorporating various particles and phases, and uses it to simulate mergers, predicting potential gravitational wave signatures of quark matter formation.

## Contribution

It introduces a unified EOS model covering subnuclear to supranuclear matter and applies it to neutron star merger simulations to identify observable signatures of quark deconfinement.

## Key findings

- EOS model includes nuclei, nucleons, hyperons, quarks
- Simulations predict gravitational wave signatures of quark matter
- Results suggest observable signals for phase transition in mergers

## Abstract

In this work, we discuss the dense matter equation of state (EOS) for the extreme range of conditions encountered in neutron stars and their mergers. The calculation of the properties of such an EOS involves modeling different degrees of freedom (such as nuclei, nucleons, hyperons, and quarks), taking into account different symmetries, and including finite density and temperature effects in a thermodynamically consistent manner. We begin by addressing subnuclear matter consisting of nucleons and a small admixture of light nuclei in the context of the excluded volume approach. We then turn our attention to supranuclear homogeneous matter as described by the Chiral Mean Field (CMF) formalism. Finally, we present results from realistic neutron-star-merger simulations performed using the CMF model that predict signatures for deconfinement to quark matter in gravitational wave signals.