Kerr-Newman-AdS Black Hole In Quintessential Dark Energy

TL;DR

This paper explores the properties of Kerr-Newman-AdS black holes influenced by quintessential dark energy, analyzing horizon structure, extremal conditions, and rotation velocities, revealing new relationships between parameters and potential astrophysical implications.

Contribution

It provides a novel analysis of Kerr-Newman-AdS black holes in quintessence fields, deriving horizon conditions, extremal black hole types, and rotation behaviors with respect to dark energy parameters.

Findings

Maximum quintessence parameter $oldsymbol{\alpha}$ varies with $oldsymbol{\omega}$ from $oldsymbol{\Lambda}$ to 1.

Black hole charge does not affect the maximum $oldsymbol{\alpha}$ value.

Rotation velocity approaches flatness for small $oldsymbol{\alpha}$, explaining galaxy rotation curves.

Abstract

Quintessential dark energy with pressure $p$ and density $\rho$ is related by equation of state $p=\omega\rho$ with the state parameter $-1<\omega<-1/3$. The cosmological dark energy influence on black hole spacetime are interesting and important. In this paper, we study the Kerr-Newman-AdS solutions of the Einstein-Maxwell equation in quintessence field around a black hole by Newman-Janis algorithm and complex computations. From the horizon structure equation, we obtain the expression between quintessence parameter $\alpha$ and cosmological constant $\Lambda$ if the black hole exists two cosmological horizon $r_{q}$ and $r_{c}$ when $\omega=-2/3$, the result is different from rotational black hole in quintessence matter situation. Through analysis we find that the black hole charge cannot change the value of $\alpha$. But the black hole spin and cosmological constant are opposite. The black hole spin and cosmological constant make the maximum value of $\alpha$ to become small. The existence of four horizon leads seven types of extremal black holes to constraint the parameter $\alpha$. With the state parameter $\omega$ ranging from $-1$ to $-1/3$, the maximum value of $\alpha$ changes from $\Lambda$ to $1$. When $\omega\rightarrow -1$, the quintessential dark energy likes cosmological constant. The singularity of the black holes is the same with that of Kerr black hole. We also discuss the rotation velocity of the black holes on the equatorial plane for $\omega=-2/3,-1/2$ and $-1/3$. For small value of $\alpha$, the rotation velocity on the equatorial plane is asymptotically flat and it can explain the rotation curves in spiral galaxies.