Matter and forces near physical black holes
arXiv:2209.10766 · doi:10.1103/PhysRevD.106.124048
Abstract
We describe general features of formation and disappearance of regular spherically symmetric black holes in semiclassical gravity. The allowed models are critically dependent on the requirement that the resulting objects evolve in finite time according to a distant observer. Violation of the null energy condition (NEC) is mandatory for this to happen, and we study the properties of the necessary energy-momentum tensor in the vicinity of the apparent horizon. In studies of the kinematics of massive test particles, it is found that the escape from a black hole is possible only on the ingoing trajectories when the particles are overtaken by the contracting outer apparent horizon. Tidal forces experienced by geodesic observers, infalling or escaping, are shown to be finite at the apparent horizon, although this is not true for nongeodesic trajectories.
arXiv comment11 pages, 3 figures. Comments welcome!
References in corpus (19)
- Observation of gravitational waves from two neutron star-black hole coalescences
- General Laws of Black-Hole Dynamics
- Warp drive basics
- Geodesically complete black holes
- Physical observability of horizons
- The Many Definitions of a Black Hole
- Versatile method for renormalized stress-energy computation in black-hole spacetimes
- Foliation dependence of black hole apparent horizons in spherical symmetry
- Renormalized stress-energy tensor for stationary black holes
- Energy-momentum tensor and metric near the Schwarzschild sphere
- Black hole evaporation and semiclassical thin shell collapse
- Closed trapping horizons without singularity
- Hawking-Ellis classification of stress-energy: test-fields versus back-reaction
- Ingoing Eddington-Finkelstein Metric of an Evaporating Black Hole
- The Vaidya metric: expected and unexpected traits of evaporating black holes
- Kerr-Vaidya black holes
- Semiclassical black holes and horizon singularities
- Paradoxes before the paradox: surface gravity and the information loss problem
- Spherically symmetric black holes in metric gravity