Gravitational collapse with non-vanishing tangential stresses II: a laboratory for cosmic censorship experiments

Abstract

The general exact solution describing the dynamics of anisotropic elastic spheres supported only by tangential stresses is reduced to a quadrature using Ori's mass-area coordinates. This leads to the explicit construction of the root equation governing the nature of the central singularity. Using this equation, we formulate and motivate on physical grounds a conjecture on the nature of this singularity. The conjecture covers a large sector of the space of initial data; roughly speaking, it asserts that addition of a tangential stress cannot undress a covered dust singularity. The root equation also allows us to analyze the case of self-similar spacetimes and to get some insight on the role of stresses in deciding the nature of the singularities in this case.

16 pages, Plain TeX format

Cited by in corpus (44)

• Recent developments in gravitational collapse and spacetime singularities
• Equilibrium configurations from gravitational collapse
• Non-singular quantum-inspired gravitational collapse
• Initial data and the end state of spherically symmetric gravitational collapse
• Expansion-Free Cavity Evolution: Some exact Analytical Models
• Strong curvature naked singularities in spherically symmetric perfect fluid collapse
• Black holes vs. naked singularities formation in collapsing Einstein's clusters
• Accretion disk luminosity for black holes surrounded by dark matter with tangential pressure
• Nakedness and curvature strength of shell-focusing singularity in the spherically symmetric space-time with vanishing radial pressure
• Gravitational collapse of barotropic spherical fluids
• The spectrum of endstates of gravitational collapse with tangential stresses
• Gravitational collapse in asymptotically Anti-de Sitter/de Sitter backgrounds
• Genericity aspects in gravitational collapse to black holes and naked singularities
• Shearfree Spherically Symmetric Fluid Models
• Global visibility of a strong curvature singularity in nonmarginally bound dust collapse
• Birth of timelike naked singularity
• Relativistic gravitational collapse in comoving coordinates: The post-quasistatic approximation
• Spherical Universes with Anisotropic Pressure
• Causal Structure of Singularity in non-spherical Gravitational Collapse
• New mathematical framework for spherical gravitational collapse
• Cosmic Censorship in Higher dimension II
• Instability of black hole formation in gravitational collapse
• General spherically symmetric elastic stars in Relativity
• Spherically symmetric steady states of John elastic bodies in general relativity
• Shell-crossings in Gravitational Collapse
• Comparing thin accretion disk properties of naked singularities and black holes
• Instability of black hole formation under small pressure perturbations
• All black holes in Lemaitre-Tolman-Bondi inhomogeneous dust collapse
• Gravitational collapse from smooth initial data with vanishing radial pressure
• Rotating elastic string loops in flat and black hole spacetimes: stability, cosmic censorship and the Penrose process
• Black hole formation from the gravitational collapse of a non-spherical network of structures
• Relativistic elasticity of rigid rods and strings
• Sufficient condition for Blackhole formation in spherical gravitational collapse
• Singularity resolution in gravitational collapse
• Collapse of spherical charged anisotropic fluid spacetimes
• High-Speed Collapse of a Hollow Sphere of Type I Matter
• Analytical solutions for black-hole critical behaviour
• Initial boundary-value problem for the spherically symmetric Einstein equations with fluids with tangential pressure
• Rebounce and Black hole formation in a Gravitational Collapse Model with Vanishing Radial Pressure
• Elastic shocks in relativistic rigid rods and balls
• Rigid elastic solids in relativity
• Can we see naked singularities?
• Geometric properties of slowly rotating black holes embedded in matter environments
• Axisymmetric Solutions to Einstein Field Equations via Integral Transforms