Stability windows for proto-quark stars

TL;DR

This paper explores the stability conditions of proto-quark stars at finite temperatures across various models, considering magnetic fields and their impact on mass-radius relations, to better understand the existence of stable strange matter.

Contribution

It introduces a comprehensive analysis of stability windows for proto-quark stars at finite temperature using multiple models, including magnetic field effects.

Findings

Stability windows depend on free energy, not just ground state energy.

Magnetic fields influence the stability and structure of proto-quark stars.

Mass-radius relations vary with temperature and magnetic field strength.

Abstract

We investigate the existence of possible stable strange matter and related stability windows at finite temperature for different models that are generally applied to describe quark stars, namely, the quark-mass density dependent model, the MIT bag model and the Nambu-Jona-Lasinio model. We emphasize that, although the limits for stable strange matter depend on a comparison with the ground state of 56Fe, which is a zero temperature state, the quantity that has to be used in the search for strange matter in proto-quark stars is the free energy and we analyze stability windows up to temperatures of the order of 40 MeV. The effects of strong magnetic fields on stability windows are computed and the resulting mass-radius relations for different stages of the proto-quark star are analyzed.