# Cooling of hypernuclear compact stars: Hartree-Fock models and high-density pairing

## TL;DR

This study investigates the cooling mechanisms of hypernuclear compact stars using covariant density functional theory, highlighting how different models affect star composition, cooling rates, and the role of high-density pairing in slowing down cooling.

## Contribution

It compares Hartree and Hartree-Fock models with various symmetry energy slopes and introduces high-density pairing effects to better understand hypernuclear star cooling.

## Key findings

- Low L models align with observed cooling data.
- High L models enable rapid cooling via direct Urca process.
- High-density pairing slows down cooling in massive stars.

## Abstract

The thermal evolution of hypernuclear compact stars is studied for stellar models constructed on the basis of covariant density functional theory in Hartree and Hartree-Fock approximation. Parametrizations of both types are consistent with the astrophysical mass constraints on compact stars and available hypernuclear data. We discuss the differences of these density functionals and highlight the effects they have on the composition and on the cooling of hypernuclear stars. It is shown that hypernuclear stars computed with density functional models that have a low symmetry energy slope, $L$, are fairly consistent with the cooling data of observed compact stars. The class of stellar models based on larger $L$ values gives rise to the direct Urca process at low densities, which leads to significantly faster cooling. We conjecture high-density pairing for protons and $\Lambda$'s in the $P$-wave channel and provide simple scaling arguments to obtain these gaps. As a consequence the most massive stellar models with masses $1.8 \le M/M_{\odot} \le2$ experience slower cooling by hyperonic dUrca processes which involve $\Lambda$'s and protons.