# Finite-temperature Equations of State for Neutron Star Mergers

## TL;DR

This paper develops finite-temperature equations of state for neutron star matter by combining nuclear and quark matter models, aiming to identify signatures of deconfined quark matter in gravitational wave signals from neutron star mergers.

## Contribution

It introduces a novel family of temperature-dependent equations of state combining nuclear and holographic quark matter models, and constrains them using recent neutron star mass measurements.

## Key findings

- Indicates a strong first order deconfinement transition at finite temperature.
- Identifies temperature-dependent critical densities and latent heat for phase transition.
- Constrains equations of state using recent neutron star mass data.

## Abstract

The detection of gravitational waves from a neutron star merger has opened up the possibility of detecting the presence or creation of deconfined quark matter using the gravitational wave signal. To investigate this possibility, we construct a family of neutron star matter equations of state at nonzero density and temperature by combining state-of-the-art nuclear matter equations of state with holographic equations of state for strongly interacting quark matter. The emerging picture consistently points toward a strong first order deconfinement transition, with a temperature-dependent critical density and latent heat that we quantitatively examine. Recent neutron star mass measurements are further used to discriminate between the different equations of state obtained, leaving a tightly constrained family of preferred equations of state.