Rotating black hole and quintessence
Centre for Theoretical Physics, Jamia Millia Islamia, New Delhi, 110025, India
2 Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag 54001, Durban, 4000, South Africa
Accepted: 30 March 2016
Published online: 22 April 2016
We discuss spherically symmetric exact solutions of the Einstein equations for quintessential matter surrounding a black hole, which has an additional parameter () due to the quintessential matter, apart from the mass (M). In turn, we employ the Newman–Janis complex transformation to this spherical quintessence black hole solution and present a rotating counterpart that is identified, for and , exactly as the Kerr–Newman black hole, and as the Kerr black hole when . Interestingly, for a given value of parameter , there exists a critical rotation parameter (), which corresponds to an extremal black hole with degenerate horizons, while for , it describes a non-extremal black hole with Cauchy and event horizons, and no black hole for . We find that the extremal value is also influenced by the parameter and so is the ergoregion.
© The Author(s), 2016