2011/06/30 by Pankaj S. Joshi, Daniele Malafarina, Ramesh Narayan
Physics and Astronomy · #gr-qc #astro-ph.HE #hep-th
paper · pdf · doi:10.1088/0264-9381/28/23/235018
published as 2011 Class. Quantum Grav. 28 235018 · 13 pages, 3 figure. Replaced with published version, several changes made according to referee's advise
arxiv created 2011/11/18 · arxiv updated 2015/05/28
We develop here a new procedure within Einstein's theory of gravity to generate equilibrium configurations that result as the final state of gravitational collapse from regular initial conditions. As a simplification, we assume that the collapsing fluid is supported only by tangential pressure. We show that the equilibrium geometries generated by this method form a subset of static solutions to the Einstein equations, and that they can either be regular or develop a naked singularity at the center. When a singularity is present, there are key differences in the properties of stable circular orbits relative to those around a Schwarzschild black hole with the same mass. Therefore, if an accretion disk is present around such a naked singularity it could be observationally distinguished from a disk around a black hole.