# Maximum mass and radius of strange stars in Finch-Skea geometry in dimensions $D\geq4$

## TL;DR

This paper models strange stars in higher-dimensional space-times using Finch-Skea geometry and MIT bag model EOS, analyzing their physical properties, stability, and maximum radii across dimensions.

## Contribution

It extends stellar modeling of strange stars to D≥4 dimensions with a specific metric and EOS, exploring maximum radii, compactness, and stability in higher dimensions.

## Key findings

- Maximum stellar radius depends on surface density and bag constant B.
- Compactness exceeds 0.33 in four dimensions and varies in higher dimensions.
- Causality and energy conditions are satisfied within the maximum radius.

## Abstract

In this article, we demonstrated a stellar model for compact star in presence of strange matter embedded in $D\ge4$ dimensional space-time defind by Finch-Skea metric. To study the relevant physical properties of the interior matter, we consider the equation of state $(henceforth~EOS)$ as proposed in MIT bag model given by $p=\frac{1}{3}(\rho-4B)$, where $B$ is termed as bag constant. The Mass-Radius relationships in four and higher dimensions are determined using the range of values of surface density through the relation $\rho_{s}=4B$ for which bulk strange matter may be a viable issue for compact objects. Here we choose the range of $B$ such that stable strange matter may exist at zero external pressure relative to neutron. We note that a maximum value of the stellar radius is exist when $B$ is fixed at a given allowed value for which metric functions considered here to be real. This is the maximum allowed radius $(b_{max})$ in this model which depends on surface density of a strange star. In four dimensions the compactness of a star is found to be greater than 0.33. In case of higher dimensions ($D>4$), we observed different values of compactness. Causality conditions are satisfied interior to the star upto maximum allowed radius $(b_{max})$ for which metric function is real. The validity of energy conditions, surface red-shift and other parameters of the stellar configuration are studied and found new results. Stability of the system is also studied.