A Bayesian study of quark models in view of recent astrophysical constraints

TL;DR

This paper uses Bayesian analysis to compare two quark star models against recent astrophysical observations, constraining their parameters to match observed pulsar masses and radii.

Contribution

It introduces a Bayesian framework to evaluate and constrain density-dependent and vector MIT bag quark models using recent astrophysical data.

Findings

Both models can produce stars with masses up to 2.35 solar masses.

Constraints restrict the parameter space of the nuclear equation of state.

Models are compatible with observed pulsar mass-radius data.

Abstract

In this work, we perform a comparative analysis between the density-dependent quark model and the vector MIT bag model using Bayesian analysis. We use the equations of state generated by these two models to describe quark stars. We impose four recent observational astrophysical constraints on both models to determine their model-dependent parameters in an optimized manner assuming that the compact objects observed are composed entirely of self-bound quarks. The restrictions are aimed at producing stars with maximum masses $2 - 2.35$ M$_\odot$ and a mass-radii diagram compatible with the observed pulsars: PSR J0740+6620, PSR J0952-0607, PSR J0030+0451 and the compact object XMMU J173203.3-344518. With this analysis, the parameter dependence of the nuclear equation of state (EoS) of both models is restricted.