The attribute of rotational profile to the hyperon puzzle in the prediction of heaviest compact star

TL;DR

This paper investigates how the rotational profile of hyperon-rich neutron stars affects the hyperon puzzle, using relativistic mean field models to predict equations of state and star properties under various conditions.

Contribution

It introduces a detailed analysis of the impact of rotational dynamics on hyperon-rich star models within an effective field theory framework, considering symmetry breaking and hyperon-meson couplings.

Findings

Rotational frequency influences star stability and structure.

Hyperon content varies with density and coupling ratios.

Predicted star masses and radii align with recent observations.

Abstract

In this theoretical study, we report an investigation of the equations of state (EoSs) ofhyper-nuclear matter and its composition as a function of density within the framework of effective field theory motivated relativistic mean field model. We have used G2 force parameter along with various hyperon-meson coupling ratios by allowing the mixing and the breaking of SU(6) symmetry to predict the EoSs, keeping the nucleonic coupling constant intact. We have estimated the properties of non-rotating and rapidly rotating configuration of compact stars by employing four different representative sets of equations of state. The obtained results of the mass and radius for the compact stars are compared with the recent mass observations. Further, we have studied the stability and sensitivity of rotational frequency (at sub-millisecond period) on the configuration of the compact stars, because the angular frequency is significantly smaller than the mass-shedding (Keplerian) frequency in slow rotation regime. Moreover, the yield of hyperon as a function of density for various hyperon-meson couplings are also estimated.