Rotating black hole and quintessence
Abstract
We discuss spherically symmetric exact solutions of the Einstein equations for quintessential matter surrounding a black hole, which has an additional parameter (ω ) due to the quintessential matter, apart from the mass ( M). In turn, we employ the NewmanJanis complex transformation to this spherical quintessence black hole solution and present a rotating counterpart that is identified, for α =e^2 ≠ 0 and ω =1/3, exactly as the KerrNewman black hole, and as the Kerr black hole when α =0. Interestingly, for a given value of parameter ω , there exists a critical rotation parameter (a=a_{E}), which corresponds to an extremal black hole with degenerate horizons, while for a<a_{E}, it describes a nonextremal black hole with Cauchy and event horizons, and no black hole for a>a_{E}. We find that the extremal value a_E is also influenced by the parameter ω and so is the ergoregion.
 Publication:

European Physical Journal C
 Pub Date:
 April 2016
 DOI:
 10.1140/epjc/s1005201640517
 arXiv:
 arXiv:1512.05476
 Bibcode:
 2016EPJC...76..222G
 Keywords:

 General Relativity and Quantum Cosmology
 EPrint:
 14 pages, 3 figures, 3 tables, accepted for publication EPJC (Letter)