Strange Stars : An interesting member of the compact object family

TL;DR

This paper investigates the properties of strange stars at various temperatures, explores their signatures in different astronomical observations, and discusses how their structural parameters can help distinguish them from neutron stars.

Contribution

It provides a detailed analysis of strange star properties using specific equations of state and solves TOV equations to understand their structure and observational signatures.

Findings

Maximum mass decreases with temperature due to softer EoS

Surface tension depends on star size and structure, exceeding conventional values

Moment of inertia can help differentiate strange stars from neutron stars

Abstract

We have studied strange star properties both at zero temperature and at finite temperatures and searched signatures of strange stars in gamma-ray, x-ray and radio astronomy. We have a set of Equations of State (EoS) for strange quark matter (SQM) and solving the TOV equations, we get the structure of strange stars. The maximum mass for a strange star decreases with the increase of temperature, because at high temperatures, the EoS become softer. One important aspect of strange star is that, surface tension depends on the size and structure of the star and is significantly larger than the conventional values. Moment of inertia is another important parameter for compact stars as by comparing theoretical values with observed estimate, it is possible to constrain the dense matter Equation of State. We hope that this approach will help us to decide whether the members of the double pulsar system PSR J0737-3039 are neutron stars or strange stars.