scholarly journals Entanglement generation outside a Schwarzschild black hole and the Hawking effect

2011 ◽  
Vol 2011 (8) ◽  
Author(s):  
Jiawei Hu ◽  
Hongwei Yu
Keyword(s):  
Black Hole ◽  
Schwarzschild Black Hole ◽  
Entanglement Generation ◽  
Hawking Effect

scholarly journals Correlation loss and multipartite entanglement across a black hole horizon (

2009 ◽  
Vol 9 (7&8) ◽  
pp. 657-665
Author(s):  
G. Adesso ◽  
I. Fuentes-Schuller
Keyword(s):  
Black Hole ◽  
Small Mass ◽  
Point Of View ◽  
Multipartite Entanglement ◽  
Squeezed State ◽  
Schwarzschild Black Hole ◽  
Bipartite Entanglement ◽  
Hawking Effect ◽  
Entanglement Distribution ◽  
Quantum And Classical Correlations

We investigate the Hawking effect on entangled fields. By considering a scalar field which is in a two-mode squeezed state from the point of view of freely falling (Kruskal) observers crossing the horizon of a Schwarzschild black hole, we study the degradation of quantum and classical correlations in the state from the perspective of physical (Schwarzschild) observers confined outside the horizon. Due to monogamy constraints on the entanglement distribution, we show that the lost bipartite entanglement is recovered as multipartite entanglement among modes inside and outside the horizon. In the limit of a small-mass black hole, no bipartite entanglement is detected outside the horizon, while the genuine multipartite entanglement interlinking the inner and outer regions grows infinitely.

scholarly journals PARTITION FUNCTION OF THE REISSNER–NORDSTRÖM BLACK HOLE

2014 ◽  
Vol 23 (01) ◽  
pp. 1450001 ◽  
Author(s):  
JARMO MÄKELÄ
Keyword(s):  
Phase Transition ◽  
Black Hole ◽  
Partition Function ◽  
Microscopic Model ◽  
Schwarzschild Black Hole ◽  
Hawking Effect ◽  
Analytic Expression

We consider a microscopic model of a stretched horizon of the Reissner–Nordström black hole. In our model, the stretched horizon consists of discrete constituents. Using our model we obtain an explicit, analytic expression for the partition function of the hole. Our partition function implies, among other things, the Hawking effect, and provides it with a microscopic explanation as a phase transition taking place at the stretched horizon. The partition function also implies the Bekenstein–Hawking entropy law. The model and its consequences are similar to those obtained previously for the Schwarzschild black hole.

scholarly journals Genuine tripartite nonlocality and entanglement in curved spacetime

2022 ◽  
Vol 82 (1) ◽  
Author(s):  
Shu-Min Wu ◽  
Hao-Sheng Zeng
Keyword(s):  
Black Hole ◽  
Hawking Temperature ◽  
Tripartite Entanglement ◽  
Schwarzschild Black Hole ◽  
Curved Spacetime ◽  
Hawking Effect ◽  
Fermion Fields ◽  
Pass Through ◽  
The One ◽  
Monogamy Relations

AbstractWe study the genuine tripartite nonlocality (GTN) and the genuine tripartite entanglement (GTE) of Dirac fields in the background of a Schwarzschild black hole. We find that the Hawking radiation degrades both the physically accessible GTN and the physically accessible GTE. The former suffers from “sudden death” at some critical Hawking temperature, and the latter approaches to the nonzero asymptotic value in the limit of infinite Hawking temperature. We also find that the Hawking effect cannot generate the physically inaccessible GTN, but can generate the physically inaccessible GTE for fermion fields in curved spacetime. These results show that on the one hand the GTN cannot pass through the event horizon of black hole, but the GTE do can, and on the other hand the surviving physically accessible GTE and the generated physically inaccessible GTE for fermions in curved spacetime are all not nonlocal. Some monogamy relations between the physically accessible GTE and the physically inaccessible GTE are found.

Quantum estimation for Dirac particles with the Hawking effect in the background of a Schwarzschild black hole

2019 ◽  
Vol 16 (8) ◽  
pp. 085206 ◽  
Author(s):  
Cheng-Cheng Liu ◽  
Jia-Dong Shi ◽  
Zhi-Yong Ding ◽  
Juan He ◽  
Tao Wu ◽  
...  
Keyword(s):  
Black Hole ◽  
Schwarzschild Black Hole ◽  
Hawking Effect ◽  
Dirac Particles

The Schwarzschild black hole

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Equilibrium Configuration ◽  
Original Form ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Metric ◽  
Schwarzschild Geometry

This chapter discusses the Schwarzschild black hole. It demonstrates how, by a judicious change of coordinates, it is possible to eliminate the singularity of the Schwarzschild metric and reveal a spacetime that is much larger, like that of a black hole. At the end of its thermonuclear evolution, a star collapses and, if it is sufficiently massive, does not become stabilized in a new equilibrium configuration. The Schwarzschild geometry must therefore represent the gravitational field of such an object up to r = 0. This being said, the Schwarzschild metric in its original form is singular, not only at r = 0 where the curvature diverges, but also at r = 2m, a surface which is crossed by geodesics.

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