Strange quark stars in modified vector MIT bag model: role of $\rho$ and $\phi$ mesons

TL;DR

This study explores how including $ ho$ and $$ mesons in a modified vector MIT bag model affects the properties of strange quark stars, revealing increased maximum mass, radius, and tidal deformability with stronger vector coupling.

Contribution

It introduces the consideration of $ ho$ and $$ vector mesons and their non-linear self-interactions into the vector MIT bag model for strange quark stars, expanding beyond previous models that only included $$ mesons.

Findings

Maximum mass of SQSs reaches 2.48 M_{\u2603} with increased vector coupling.

Radii of SQSs are approximately 12.2 km for high-mass configurations.

Tidal deformability increases with vector coupling, especially for low-mass stars.

Abstract

In the present work, we study the properties of strange quark stars (SQSs) using the vector MIT bag model with modification in vector channels. Unlike recent studies which only consider interactions through $\omega$ mesons, we analyze the possibility of $\rho$ and $\phi$ vector channels. We consider two types of higher order non-linear self-interaction terms for the vector mesons. With these modifications, we computed the equation of state (EoS) and mass-radius of strange stars for different values of vector coupling strength. Considerations of $\rho$ and $\phi$ vector mesons along with $\omega$, as well as an increase in the strength of vector coupling $g_v$, enhance the mass and radius of SQSs. For two kind of non-linear self-interactions of vector mesons considered in the present calculations, we observe the SQSs with maximum mass $2.48$ and $2.42 M_{\odot}$ for the vector coupling $g_v = 3$. Corresponding radii of these SQSs are found to be $12.27$ and $12.18$ km, respectively. We also calculate the tidal deformability parameter $\Lambda$, the Love number $k_2$ and the gravitational redshift of SQSs. The tidal deformability parameter $\Lambda$ is observed to increase with $g_v$, with appreciable effect for low mass stars.