2004/06/12 by Rituparno Goswami, Pankaj S. Joshi, Pankaj S Joshi · 2 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Quantum chaos and dynamical systems #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1088/0264-9381/21/15/002
published as Class.Quant.Grav. 21 (2004) 3645-3654 · 7 Pages, Revtex4, To appear in Classical and Quantum Gravity
arxiv created 2004/06/12 · openalex publication_date 2004/07/09 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We investigate here the gravitational collapse end states for a spherically symmetric perfect fluid with an equation of state p = k ρ. It is shown that given regular initial data in terms of the density and pressure profiles at the initial epoch from which the collapse develops, the black-hole or naked singularity outcomes depend on the choice of rest of the free functions available, such as the velocities of the collapsing shells and the dynamical evolutions as allowed by the Einstein equations. This clarifies the role that equation of state and initial data play in determining the final fate of gravitational collapse.