# Simplified Thermal Evolution of Proto-hybrid Stars

## TL;DR

This paper investigates the thermal evolution and phase transition of proto-hybrid stars, analyzing their maximum mass and potential late phase transition from hadronic to quark matter, with implications for observed neutron star masses.

## Contribution

It introduces a model for the thermal evolution of proto-hybrid stars considering finite temperature effects and phase transitions, providing new insights into their maximum mass and evolution.

## Key findings

- Cold hybrid stars can have masses ≥ 2 solar masses.
- A late phase transition during proto-hybrid star evolution is possible.
- The study aligns hybrid star properties with observed pulsar constraints.

## Abstract

We study the possibility of a hadron-quark phase transition in the interior of neutron stars, taking into account different schematic evolutionary stages at finite temperature. Furthermore, we analyze the astrophysical properties of hot and cold hybrid stars, considering the constraint on maximum mass given by the pulsars J1614-2230 and J1614-2230. We obtain cold hybrid stars with maximum masses $\geq 2$ M$_{\odot}$. Our study also suggest that during the proto-hybrid star evolution a late phase transition between hadronic matter and quark matter could occur, in contrast with previous studies of proto-neutron stars.