Rotating black hole solutions with quintessential energy

Understand

Quintessential dark energy with density $\rho$ and pressure $p$ is governed by an equation of state of the form $p=-\omega_{q}\rho$ with the quintessential parameter $\omega_q\in(-1;-1/3)$.

• We derive the geometry of quintessential rotating black holes, generalizing thus the Kerr spacetimes.
• Then we study the quintessential rotating black hole spacetimes with the special value of $\omega_q = -2/3$ when the resulting formulae are simple and easily tractable.
• We show that such special spacetimes can exist for dimensionless quintessential parameter $c<1/6$ and determine the critical rotational parameter $a_0$ separating the black hole and naked singularity spacetime in dependence on the quintessential parameter $c$.