Method to compute the stress-energy tensor for a quantized scalar field when a black hole forms from the collapse of a null shell
arXiv:2009.03453 · doi:10.1103/PhysRevD.102.125035
Abstract
A method is given to compute the stress-energy tensor for a massless minimally coupled scalar field in a spacetime where a black hole forms from the collapse of a spherically symmetric null shell in four dimensions. Part of the method involves matching the modes for the in vacuum state to a complete set of modes in Schwarzschild spacetime. The other part involves subtracting from the unrenormalized expression for the stress-energy tensor when the field is in the in vacuum state, the corresponding expression when the field is in the Unruh state and adding to this the renormalized stress-energy tensor for the field in the Unruh state. The method is shown to work in the two-dimensional case where the results are known.
arXiv comment40 pages, 4 figures
References in corpus (16)
- Semiclassical Stability of the Extreme Reissner-Nordstrom Black Hole
- Semiclassical Extremal Blackholes
- Lagrange Inversion
- Versatile method for renormalized stress-energy computation in black-hole spacetimes
- Hawking radiation and secularly growing loop corrections
- Mirror Reflections of a Black Hole
- Renormalized stress-energy tensor of an evaporating spinning black hole
- Quantum fluxes at the inner horizon of a spherical charged black hole
- Renormalized stress-energy tensor for stationary black holes
- The Renormalized Stress Tensor in Kerr Space-Time: Numerical Results for the Hartle-Hawking Vacuum
- Cutoff AdS/CFT duality and the quest for braneworld black holes
- Low frequency gray-body factors and infrared divergences: rigorous results
- Hawking radiation correlations in Bose Einstein condensates using quantum field theory in curved space
- Hadamard Renormalization of the Stress Energy Tensor in a Spherically Symmetric Black Hole Space-Time with an Application to Lukewarm Black Holes
- Stress-Energy Tensor for the Massless Spin 1/2 Field in Static Black Hole Spacetimes
- Late time approach to Hawking radiation: terms beyond leading order
Cited by in corpus (5)
- Semiclassical relativistic stars
- Evaporation of four-dimensional dynamical black holes sourced by the quantum trace anomaly
- Hadamard states on spherically symmetric characteristic surfaces, the semi-classical Einstein equations and the Hawking effect
- Infrared Effects and the Unruh State
- Computation of the semiclassical outflux emerging from a collapsing spherical null shell