Compact star merger events with stars composed of interacting strange quark matter

TL;DR

This study models strange quark matter stars to analyze their properties during merger events, aligning with recent gravitational wave and astrophysical observations, and provides new bounds on their deformability and radii.

Contribution

It introduces new models of strange quark matter stars considering interactions, and derives updated bounds on their tidal deformability and radii consistent with observational data.

Findings

New upper bound on tidal deformability for 1.4 solar mass strange stars.

Range of compactness for 1.4 solar mass strange stars: 0.175 to 0.199.

Radius constraints for 1.5 and 1.7 solar mass strange stars.

Abstract

We investigate the properties of stars participating in double compact star merger events considering interacting model of stable strange quark matter. We model the matter making it compatible with the recent astrophysical observations of compact star mass-radius and gravitational wave events. In this context we consider modified MIT bag model and vector bag model with and without self interaction. We find new upper bound on tidal deformability of $1.4~M_\odot$ strange star corresponding to the upper bound of effective tidal deformability inferred from gravitational wave event. Range of compactness of $1.4~M_\odot$ strange star is obtained as ${0.175}\leq{C_{1.4}}\leq{0.199}$. Radius range of $1.5M_\odot$ primary star is deduced to be ${10.57}\leq{R_{1.5}}\leq{12.04}$ km, following stringent GW170817 constraints. GW190425 constraints provide with upper limit on radius of $1.7$ solar mass strange star that it should be less than $13.41$ $\text{km}$.