Self-consistent description of a spherically-symmetric gravitational collapse

Abstract

In spherical symmetry, the total energy-momentum tensor near the apparent horizon is identified up to a single function of time from two assumptions: a trapped region forms at a finite time of a distant observer, and values of two curvature scalars are finite at its boundary. In general relativity, this energy-momentum tensor leads to the unique limiting form of the metric. The null energy condition is violated across the apparent horizon and is satisfied in the vicinity of the inner apparent horizon. As a result, homogenous collapse models cannot describe the formation of a black hole. Properties of matter change discontinuously immediately after formation of a trapped region. Absolute values of comoving density, pressure, and flux coincide at the apparent horizon. Thus, collapse of ideal fluids cannot lead to the formation of black holes. Moreover, these three quantities diverge at the expanding apparent horizon, producing a regular (i.e., finite curvature) firewall. This firewall is incompatible with quantum energy inequalities, implying that trapped regions, once formed at some finite time of a distant observer, cannot grow.

7 pages, 1 figure. Published version [with a slightly better notation]

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Cited by in corpus (17)

• Testing the nature of dark compact objects: a status report
• Energy conditions in general relativity and quantum field theory
• Equilibrium, radial stability and non-adiabatic gravitational collapse of anisotropic neutron stars
• Black hole evaporation and semiclassical thin shell collapse
• Pandora's box lid: geometry near the apparent horizon
• Universal properties of the near-horizon geometry
• Kerr-Vaidya black holes
• Semiclassical black holes and horizon singularities
• Paradoxes before the paradox: surface gravity and the information loss problem
• Black holes as spherically-symmetric horizon-bound objects
• Planckian Physics Comes Into Play At Planckian Distance From Horizon
• Physical black holes in fourth-order gravity
• Spherically symmetric black holes in metric gravity
• Physical black holes in semiclassical gravity
• Horizon-bound objects: Kerr--Vaidya solutions
• Black holes and their horizons in semiclassical and modified theories of gravity
• Alternative characterization of a black hole boundary