scholarly journals Near-extremal black hole evaporation in asymptotically flat spacetime

2002 ◽  
Vol 66 (2) ◽  
Author(s):  
Kamran Diba ◽  
David A. Lowe
Keyword(s):  
Black Hole ◽  
Extremal Black Hole ◽  
Black Hole Evaporation ◽  
Asymptotically Flat ◽  
Flat Spacetime

scholarly journals Islands and stretched horizon

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Yoshinori Matsuo
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Entanglement Entropy ◽  
Total System ◽  
Island Rule ◽  
Asymptotically Flat ◽  
Flat Spacetime ◽  
Ads Spacetime ◽  
Hole Geometry

Abstract Recently it was proposed that the entanglement entropy of the Hawking radiation contains the information of a region including the interior of the event horizon, which is called “island.” In studies of the entanglement entropy of the Hawking radiation, the total system in the black hole geometry is separated into the Hawking radiation and black hole. In this paper, we study the entanglement entropy of the black hole in the asymptotically flat Schwarzschild spacetime. Consistency with the island rule for the Hawking radiation implies that the information of the black hole is located in a different region than the island. We found an instability of the island in the calculation of the entanglement entropy of the region outside a surface near the horizon. This implies that the region contains all the information of the total system and the information of the black hole is localized on the surface. Thus the surface would be interpreted as the stretched horizon. This structure also resembles black holes in the AdS spacetime with an auxiliary flat spacetime, where the information of the black hole is localized at the interface between the AdS spacetime and the flat spacetime.

An Intuitive Understanding of Black-Hole Evaporation by Viewing it in Terms of More Familiar Quantum-Field Effects in Flat Spacetime

1987 ◽  
Vol 42 (7) ◽  
pp. 657-662
Author(s):  
R. M. Nugayev
Keyword(s):  
Black Hole ◽  
Potential Barrier ◽  
Casimir Effect ◽  
Field Potential ◽  
Particle Creation ◽  
Positive Energy ◽  
Quantum Field ◽  
Black Hole Evaporation ◽  
Flat Spacetime ◽  
Field Effects

The article is aimed at an intuitive understanding of the recently explored deep connections between therm al physics, quantum field theory and general relativity. The physical effects involved in particle creation by a black hole are viewed in terms of more familiar quantum -field effects in flat spacetime. Black hole evaporation is investigated in terms of temperature correction to the Casimir effect. T he application of the Casimir effect results and those for accelerated mirrors reveals that a black hole should produce the blackbody radiation at a temperature that exactly coincides with Hawking’s result. Its blackbody nature is due to the interaction of virtual positive-energy particles with the surface of a “cavity” formed by the Schwarzchild gravitational field potential barrier. The virtual particles are “squeezed out” by the contraction of the potential barrier and appear to an observer at J+ as the real blackbody ones.

scholarly journals Phase transition to a hairy black hole in asymptotically flat spacetime

2013 ◽  
Vol 2013 (11) ◽  
Author(s):  
Theodoros Kolyvaris ◽  
George Koutsoumbas ◽  
Eleftherios Papantonopoulos ◽  
George Siopsis
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Asymptotically Flat ◽  
Flat Spacetime ◽  
Hairy Black Hole

scholarly journals Quasilocal Smarr relation for an asymptotically flat spacetime

2021 ◽  
Vol 81 (4) ◽  
Author(s):  
Yein Lee ◽  
Matthew Richards ◽  
Sean Stotyn ◽  
Miok Park
Keyword(s):  
Black Hole ◽  
Surface Pressure ◽  
Thermodynamic Potential ◽  
Black Hole Thermodynamics ◽  
Dilaton Field ◽  
Asymptotically Flat ◽  
Flat Spacetime ◽  
Euler’S Theorem ◽  
Pressure Term ◽  
Black Hole Solutions

AbstractWe investigate the thermodynamics of Einstein–Maxwell (-dilaton) theory for an asymptotically flat spacetime in a quasilocal frame. We firstly define a quasilocal thermodynamic potential via the Euclidean on-shell action and formulate a quasilocal Smarr relation from Euler’s theorem. Then we calculate the quasilocal energy and surface pressure by employing a Brown–York quasilocal method along with Mann–Marolf counterterm and find entropy from the quasilocal thermodynamic potential. These quasilocal variables are consistent with the Tolman temperature and the entropy in a quasilocal frame turns out to be same as the Bekenstein–Hawking entropy. As a result, we found that a surface pressure term and its conjugate variable, a quasilocal area, do not participate in a quasilocal thermodynamic potential, but should be present in a quasilocal Smarr relation and the quasilocal first law of black hole thermodynamics. For dyonic black hole solutions having dynamic dilaton field, a non-trivial dilaton contribution should occur in the quasilocal first law but not in the quasilocal Smarr relation.

scholarly journals Entanglement entropy of asymptotically flat non-extremal and extremal black holes with an island

2021 ◽  
Vol 81 (10) ◽  
Author(s):  
Wontae Kim ◽  
Mungon Nam
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Entanglement Entropy ◽  
Heat Bath ◽  
Extremal Black Hole ◽  
Curvature Singularity ◽  
Island Rule ◽  
Generalized Entropy ◽  
Asymptotically Flat ◽  
Extremal Black Holes

AbstractThe island rule for the entanglement entropy is applied to an eternal Reissner–Nordström black hole. The key ingredient is that the black hole is assumed to be in thermal equilibrium with a heat bath of an arbitrary temperature and so the generalized entropy is treated as being off-shell. Taking the on-shell condition to the off-shell generalized entropy, we find the generalized entropy and then obtain the entanglement entropy following the island rule. For the non-extremal black hole, the entanglement entropy grows linearly in time and can be saturated after the Page time as expected. The entanglement entropy also has a well-defined Schwarzschild limit. In the extremal black hole, the island prescription provides a logarithmically growing entanglement entropy in time and a constant entanglement entropy after the Page time. In the extremal black hole, the boundary of the island hits the curvature singularity where the semi-classical approximations appear invalid. To avoid encountering the curvature singularity, we apply this procedure to the Hayward black hole regular at the origin. Consequently, the presence of the island in extremal black holes can provide a finite entanglement entropy, which might imply non-trivial vacuum configurations of extremal black holes.

scholarly journals Soft photon theorem in the small negative cosmological constant limit

2021 ◽  
Vol 2021 (8) ◽  
Author(s):  
Nabamita Banerjee ◽  
Karan Fernandes ◽  
Arpita Mitra
Keyword(s):  
Cosmological Constant ◽  
Tree Level ◽  
Leading Order ◽  
Asymptotically Flat ◽  
Soft Factor ◽  
Flat Spacetime ◽  
Electromagnetic Interactions ◽  
Flat Spacetimes ◽  
Perturbative Corrections ◽  
Soft Factors

Abstract We study the effect of electromagnetic interactions on the classical soft theorems on an asymptotically AdS background in 4 spacetime dimensions, in the limit of a small cosmological constant or equivalently a large AdS radius l. This identifies 1/l2 perturbative corrections to the known asymptotically flat spacetime leading and subleading soft factors. Our analysis is only valid to leading order in 1/l2. The leading soft factor can be expected to be universal and holds beyond tree level. This allows us to derive a 1/l2 corrected Ward identity, following the known equivalence between large gauge Ward identities and soft theorems in asymptotically flat spacetimes.

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