Kerr-Newman-AdS black hole in quintessential dark energy

Abstract

Quintessential dark energy with pressure p and density ρ is related by equation of state p = ωρ with the state parameter −1 < ω < −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 α and cosmological constant Λ if the black hole exists two cosmological horizon r q and r c when ω = −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 α. But the black hole spin and cosmological constant are opposite. The black hole spin and cosmological constant make the maximum value of α to become small. The existence of four horizon leads seven types of extremal black holes to constraint the parameter α. With the state parameter ω ranging from −1 to −1/3, the maximum value of α changes from Λ to 1. When ω → −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 ω = −2/3, −1/2 and −1/3. For small value of α, the rotation velocity on the equatorial plane is asymptotically flat and it can explain the rotation curves in spiral galaxies.

Shadow and quasinormal modes of a rotating loop quantum black hole

“…Recently, one of us has proposed a new procedure [77,78], in which one simply drops the complexification step of the Newman-Janis algorithm. The procedure has been applied to various cases [27,40,[77][78][79][80][81][82][83][84][85][86][87][88][89][90][91][92][93][94][95][96]. One of the main purposes of this paper is to construct the rotating LQBH solution by using this new procedure, and then to investigate its main geometric properties and the effects of LQG on the shadow of the rotating LQBH solution.…”

Rotating black holes with an anisotropic matter field

“…(21) reduces to those of Kerr-Newman black hole. The components G tφ and G φφ are different from the previous results in [20,21]. Let us consider physical quantities in an orthonormal frame, (et, er, eθ, eφ) in Refs.…”

“…First, we construct a rotating geometry and then obtain matter field satisfying the Einstein equations. For the first step, we employ the Newman-Janis (NJ) algorithm [17,18,19], which has become popular to study the rotational geometry [20,21,22,23,24,25]. This algorithm generates a rotating geometry from a known static one.…”

Higgs masses and couplings in a general 2HDM with unitarity bounds

“…[3,4], which we have implemented in our numerical calculations [2]. Also we apply conditions [5], which guarantee that the vacuum state has a lower value of the potential than all the other possible stability points of the potential.…”