Relativistic harmonic oscillator model for quark stars

TL;DR

This paper applies the relativistic harmonic oscillator model to quark stars, deriving their mass-radius relationship and comparing it with the bag model, highlighting differences in stability conditions and physical properties.

Contribution

It introduces the RHO model for quark stars, incorporating confinement effects into the degenerate pressure, and compares its predictions with the traditional bag model.

Findings

Masses and radii are larger in RHO model.

Lower central energy densities are needed for stability in RHO model.

Qualitative similarity but quantitative differences with bag model.

Abstract

The relativistic harmonic oscillator (RHO) model of hadrons is used to study quark stars. The mass-radius relationship is obtained and compared with bag model of quark star, using Tolman-Oppenheimer-Volkoff equation. In this model, the outward degenerate pressure due to discrete Landau levels and Landau degeneracy balances the inward gravitational pressure. Where as in bag model the degenerate pressure is due to the standard continuum levels which balances the combined inward pressure due to gravitation and bag pressure. So in RHO model, the confinement effect is included in the degenerate pressure. We found a qualitative similarity, but quantitative differences in mass-radius relationship of quark stars in these two models. Masses and radii are relatively larger and the central energy densities, required for stable quark stars, are lower in RHO model than that of bag model.