# Rotating hybrid stars with the Dyson-Schwinger quark model

## TL;DR

This paper investigates the properties of rapidly rotating hybrid stars using advanced quark and nuclear matter models, analyzing their maximum mass, size, and spin behavior, and comparing results with observational data.

## Contribution

It introduces a combined approach using the Dyson-Schwinger model and Brueckner-Hartree-Fock theory to study rotating hybrid stars, including their rotational evolution and stability.

## Key findings

- Maximum gravitational mass and radius determined for stable configurations.
- Identification of a spinup phenomenon in supramassive stars.
- Comparison of theoretical models with observational constraints.

## Abstract

We study rapidly rotating hybrid stars with the Dyson-Schwinger model for quark matter and the Brueckner-Hartree-Fock many-body theory with realistic two-body and three-body forces for nuclear matter. We determine the maximum gravitational mass, equatorial radius, and rotation frequency of stable stellar configurations by considering the constraints of the Keplerian limit and the secular axisymmetric instability, and compare with observational data. We also discuss the rotational evolution for constant baryonic mass, and find a spinup phenomenon for supramassive stars before they collapse to black holes.