Abstract
We investigate the consequences of the collapse-induced radiation anticipated before formation of the event horizon. After reviewing the principles underlying semi-classical analysis of black holes we illustrate them by modelling collapse of evaporating massive thin dust shells using two families of metrics for the exterior geometry: the outgoing Vaidya metric and the retarded Schwarzschild metric. We describe how hypothetical pre-Hawking radiation modifies the equation of motion for the shell. Provided that a non-zero radiation flux is perceived by a distant observer, the shell never gets closer than a certain sub-Planckian distance from the Schwarzschild radius. This distance depends only on the shell's mass and evaporation rate. The stress-energy tensor is everywhere finite, but a comoving observer encounters firewall-like energy density and flux. We emphasize the logical connections between different assumptions within the semi-classical approach and discuss consequences of the apparent contradictions between them.
| Language | English |
|---|---|
| Article number | 185005 |
| Pages | 1-25 |
| Number of pages | 25 |
| Journal | Classical and Quantum Gravity |
| Volume | 35 |
| Issue number | 18 |
| DOIs | |
| Publication status | Published - 17 Aug 2018 |
Keywords
- thin shells
- pre-Hawking radiation
- collapse
Cite this
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Role of evaporation in gravitational collapse. / Baccetti, Valentina; Mann, Robert B.; Terno, Daniel R.
In: Classical and Quantum Gravity, Vol. 35, No. 18, 185005, 17.08.2018, p. 1-25.Research output: Contribution to journal › Article › Research › peer-review
TY - JOUR
T1 - Role of evaporation in gravitational collapse
AU - Baccetti, Valentina
AU - Mann, Robert B.
AU - Terno, Daniel R.
PY - 2018/8/17
Y1 - 2018/8/17
N2 - We investigate the consequences of the collapse-induced radiation anticipated before formation of the event horizon. After reviewing the principles underlying semi-classical analysis of black holes we illustrate them by modelling collapse of evaporating massive thin dust shells using two families of metrics for the exterior geometry: the outgoing Vaidya metric and the retarded Schwarzschild metric. We describe how hypothetical pre-Hawking radiation modifies the equation of motion for the shell. Provided that a non-zero radiation flux is perceived by a distant observer, the shell never gets closer than a certain sub-Planckian distance from the Schwarzschild radius. This distance depends only on the shell's mass and evaporation rate. The stress-energy tensor is everywhere finite, but a comoving observer encounters firewall-like energy density and flux. We emphasize the logical connections between different assumptions within the semi-classical approach and discuss consequences of the apparent contradictions between them.
AB - We investigate the consequences of the collapse-induced radiation anticipated before formation of the event horizon. After reviewing the principles underlying semi-classical analysis of black holes we illustrate them by modelling collapse of evaporating massive thin dust shells using two families of metrics for the exterior geometry: the outgoing Vaidya metric and the retarded Schwarzschild metric. We describe how hypothetical pre-Hawking radiation modifies the equation of motion for the shell. Provided that a non-zero radiation flux is perceived by a distant observer, the shell never gets closer than a certain sub-Planckian distance from the Schwarzschild radius. This distance depends only on the shell's mass and evaporation rate. The stress-energy tensor is everywhere finite, but a comoving observer encounters firewall-like energy density and flux. We emphasize the logical connections between different assumptions within the semi-classical approach and discuss consequences of the apparent contradictions between them.
KW - thin shells
KW - pre-Hawking radiation
KW - collapse
UR - http://www.scopus.com/inward/record.url?scp=85053142130&partnerID=8YFLogxK
U2 - 10.1088/1361-6382/aad70e
DO - 10.1088/1361-6382/aad70e
M3 - Article
VL - 35
SP - 1
EP - 25
JO - Classical and Quantum Gravity
T2 - Classical and Quantum Gravity
JF - Classical and Quantum Gravity
SN - 0264-9381
IS - 18
M1 - 185005
ER -