Dark Matter Influence on Quarkyonic Stars: A Relativistic Mean Field Analysis

TL;DR

This paper investigates how dark matter influences the structure of quarkyonic stars using a relativistic mean-field approach, demonstrating that dark matter softens the equation of state and affects observable neutron star properties.

Contribution

It introduces a model incorporating dark matter into quarkyonic matter within neutron stars, analyzing its impact on the star's equation of state and macroscopic properties using RMF formalism.

Findings

Dark matter softens the equation of state of quarkyonic matter.

The combination of quarkyonic matter and dark matter aligns with observational constraints.

Parameter variations provide insights into neutron star properties and dark matter characteristics.

Abstract

The formulation of quarkyonic matter consists of treating both quarks and nucleons as quasi-particles, where a cross-over transition occurs between the two phases. This work is based upon some of the early ideas of quark matter. It can satisfy the different observational constraints on the neutron star (NS), such as its maximum mass and the canonical radius. In addition, we put an extra component inside the NS known as Dark Matter (DM) because it is trapped due to its immense gravitational potential. In this work, we explore the impact of fermionic DM on the structure of the NS. The equation of state (EOS) is derived for the NS with the quarkyonic matter by assuming that nucleons and quarks are in equilibrium, followed by the relativistic mean-field (RMF) formalism. The recently modeled two parameterizations, such as G3 and IOPB-I, are taken to calculate the various macroscopic properties of the NS. The three unknown parameters such as the transition density ($n_t$), the QCD confinement scale ($\Lambda_{\rm sc}$), and the DM Fermi momentum ($k_f^{\rm DM}$) are varied to obtain the NS properties. The quarkyonic matter stiffens the EOS while DM softens it. The mutual combination provides us with good theoretical predictions for the magnitude of macroscopic properties consistent with the different observational results. Also, one can estimate the parameters of the DM admixed quarkyonic star with different statistical analyses, which can be further used to explore the other properties of the quarkyonic star.