Vacuum-dual static perfect fluid obeying $p=-(n-3)\rho/(n+1)$ in $n(\ge 4)$ dimensions

TL;DR

This paper derives higher-dimensional static perfect fluid solutions with a specific linear equation of state, exploring their properties, dualities, and potential to form regular or bounce black hole configurations.

Contribution

It generalizes Semiz's four-dimensional solution to higher dimensions, classifies solutions into two classes, and investigates their horizon regularity and physical implications.

Findings

Class-I solutions are dual to topological Schwarzschild-(A)dS solutions.

For n=4, solutions are smooth at horizons; for n≥6, horizons become curvature singularities.

Certain configurations allow regular black holes or big-bounce scenarios inside horizons.

Abstract

We obtain the general $n(\ge 4)$-dimensional static solution with an $(n-2)$-dimensional Einstein base manifold for a perfect fluid obeying a linear equation of state $p=-(n-3)\rho/(n+1)$. It is a generalization of Semiz's four-dimensional general solution with spherical symmetry and consists of two different classes. Through the Buchdahl transformation, the class-I and class-II solutions are dual to the topological Schwarzschild-Tangherlini-(A)dS solution and one of the $\Lambda$-vacuum direct-product solutions, respectively. While the metric of the spherically symmetric class-I solution is $C^\infty$ at the Killing horizon for $n=4$ and $5$, it is $C^1$ for $n\ge 6$ and then the Killing horizon turns to be a parallelly propagated curvature singularity. For $n=4$ and $5$, the spherically symmetric class-I solution can be attached to the Schwarzschild-Tangherlini vacuum black hole with the same value of the mass parameter at the Killing horizon in a regular manner, namely without a lightlike massive thin-shell. This construction allows new configurations of an asymptotically (locally) flat black hole to emerge. If a static perfect fluid hovers outside a vacuum black hole, its energy density is negative. In contrast, if the dynamical region inside the event horizon of a vacuum black hole is replaced by the class-I solution, the corresponding matter field is an anisotropic fluid and may satisfy the null and strong energy conditions. While the latter configuration always involves a spacelike singularity inside the horizon for $n=4$, it becomes a non-singular black hole of the big-bounce type for $n=5$ if the ADM mass is larger than a critical value.