Quasi-Local Energy of a Rotating Object Described by Kerr Spacetime

Abstract

The Brown-York quasi-local energy of a rotating black hole described by the Kerr metric and enclosed by a fixed-radius surface is calculated by direct computation. No special assumptions on the angular momentum or the radial coordinate in Boyer-Lindquist coordinates were placed. The arbitrary reference term has been set to zero. The result may be relevant for applications in astrophysics, for modeling elementary particles or for extensions of the framework of quasi-local quantities. An analytic expression in terms of incomplete elliptic integrals is given.

9 pages, 6 figures

References in corpus (6)

• The Kerr spacetime: A brief introduction
• Note on counterterms in asymptotically flat spacetimes
• Self-Renormalization of the Classical Quasilocal Energy
• First order perturbations of the Einstein-Straus and Oppenheimer-Snyder models
• Wang and Yau's Quasi-Local Energy for an Extreme Kerr Spacetime
• Quasilocal energy and surface geometry of Kerr spacetime

Cited by in corpus (3)

• Quasi-Local Energy of a Charged Rotating Object Described by the Kerr-Newman Metric
• Quasilocal Smarr relations for static black holes
• Note on the Conservation of Quasi-Local Energy in an Expanding Universe