Instability of black hole formation under small pressure perturbations

Abstract

We investigate here the spectrum of gravitational collapse endstates when arbitrarily small perfect fluid pressures are introduced in the classic black hole formation scenario as described by Oppenheimer, Snyder and Datt (OSD) [1]. This extends a previous result on tangential pressures [2] to the more physically realistic scenario of perfect fluid collapse. The existence of classes of pressure perturbations is shown explicitly, which has the property that injecting any smallest pressure changes the final fate of the dynamical collapse from a black hole to a naked singularity. It is therefore seen that any smallest neighborhood of the OSD model, in the space of initial data, contains collapse evolutions that go to a naked singularity outcome. This gives an intriguing insight on the nature of naked singularity formation in gravitational collapse.

7 pages, 1 figure, several modifications to match published version on GRG

References in corpus (8)

• Recent developments in gravitational collapse and spacetime singularities
• Spherical gravitational collapse in N-dimensions
• Gravitational collapse of homogeneous scalar fields
• Naked singularities as particle accelerators
• Naked Singularities as Particle Accelerators II
• Critical Collapse of a Complex Scalar Field with Angular Momentum
• On critical collapse of gravitational waves
• Instability of black hole formation in gravitational collapse

Cited by in corpus (7)

• Probing the space-time geometry around black hole candidates with the resonance models for high-frequency QPOs and comparison with the continuum-fitting method
• Testing the Kerr black hole hypothesis
• Strong curvature naked singularities in spherically symmetric perfect fluid collapse
• Collapse and dispersal of a homogeneous spin fluid in Einstein-Cartan theory
• Gravitational Collapse of Baryonic and Dark matter
• All black holes in Lemaitre-Tolman-Bondi inhomogeneous dust collapse
• Nakedly singular counterpart of Schwarzschild's incompressible star. A barotropic continuity condition in the center