Analytical model on mass limit of strange stars

TL;DR

This paper introduces a new analytical stellar model using the Nariai IV metric to study strange stars, establishing a maximum stable mass of approximately 1.92 solar masses, and providing insights into their mass-radius relationship.

Contribution

The paper develops a novel analytical model for strange stars based on the Nariai IV metric, offering stability conditions and mass limits not previously detailed.

Findings

Strange stars up to 1.9165 solar masses are stable.

The model predicts a maximum stable mass for strange stars.

Applicable to predicting radii of high-mass strange stars.

Abstract

In this paper, we present a new kind of stellar model using the Nariai IV metric. This model can be used to study the strange/quark stars(which is our present interest, though it can also be applicable to neutron stars). We present a mass-radius region where all the regularity conditions, energy conditions, the TOV equation, and stability conditions are satisfied. According to our model, strange stars having mass up to $1.9165M_{\odot}(=2.81 km)$ is stable. A strange star having a mass greater than $1.9165M_{\odot}$ violates the stability conditions. This model can be very useful to predict the radius of strange stars of mass greater than $1 M_{\odot}$.