# Neutron star cooling with microscopic equations of state

## TL;DR

This paper models neutron star cooling using various microscopic equations of state, demonstrating that all models can fit observed cooling data if specific superfluid gaps are assumed, and analyzes the resulting neutron star mass distributions.

## Contribution

It introduces multiple microscopic nuclear equations of state compatible with recent neutron star merger data and assesses their implications for neutron star cooling and mass distribution.

## Key findings

- All models fit current cooling data with appropriate superfluid gaps.
- Models predict neutron star mass distributions, identifying preferred ones.
- Strong direct Urca processes are present in all models.

## Abstract

We model neutron star cooling with several microscopic nuclear equations of state based on different nucleon-nucleon interactions and three-body forces, and compatible with the recent GW170817 neutron star merger event. They all feature strong direct Urca processes. We find that all models are able to describe well the current set of cooling data for isolated neutron stars, provided that large and extended proton 1S0 gaps and no neutron 3PF2 gaps are active in the stellar matter. We then analyze the neutron star mass distributions predicted by the different models and single out the preferred ones.