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.

DE SITTER-SCHWARZSCHILD BLACK HOLE: ITS PARTICLELIKE CORE AND THERMODYNAMICAL PROPERTIES

1996 ◽  
Vol 05 (05) ◽  
pp. 529-540 ◽  
Author(s):  
I.G. DYMNIKOVA
Keyword(s):  
Black Hole ◽  
Lower Limit ◽  
Mass Parameter ◽  
Hawking Temperature ◽  
Einstein Equations ◽  
Black Hole Mass ◽  
De Sitter ◽  
Schwarzschild Black Hole ◽  
Schwarzschild Solution ◽  
Second Order Phase Transition

We analyze the globally regular solution of the Einstein equations describing a black hole whose singularity is replaced by the de Sitter core. The de Sitter—Schwarzschild black hole (SSBH) has two horizons. Inside of it there exists a particlelike structure hidden under the external horizon. The critical value of mass parameter M cr1 exists corresponding to the degenerate horizon. It represents the lower limit for a black-hole mass. Below M cr1 there is no black hole, and the de Sitter-Schwarzschild solution describes a recovered particlelike structure. We calculate the Hawking temperature of SSBH and show that specific heat is broken and changes its sign at the value of mass M cr 2>M cr 1 which means that a second-order phase transition occurs at that point. We show that the Hawking temperature drops to zero when a mass approaches the lower limit M cr1 .

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 Rotating Disc around a Schwarzschild Black Hole

Universe ◽  
2020 ◽  
Vol 6 (2) ◽  
pp. 27 ◽  
Author(s):  
Oldřich Semerák ◽  
Pavel Čížek
Keyword(s):  
Black Hole ◽  
Surface Density ◽  
Schwarzschild Black Hole ◽  
Rotating Disc ◽  
First Order ◽  
Thin Disc ◽  
Thin Ring ◽  
Extended Sources ◽  
The One ◽  
First Order Perturbation

A stationary and axisymmetric (in fact circular) metric is reviewed which describes the first-order perturbation of a Schwarzschild black-hole space-time due to a rotating finite thin disc encircling the hole symmetrically. The key Green functions of the problem (corresponding to an infinitesimally thin ring)—the one for the gravitational potential and the one for the dragging angular velocity—were already derived, in terms of infinite series, by Will in 1974, but we have now put them into closed forms using elliptic integrals. Such forms are more practical for numerical evaluation and for integration in problems involving extended sources. This last point mostly remains difficult, but we illustrate that it may be workable by using the simple case of a finite thin disc with constant Newtonian surface density.

Physics in Curved Spacetime

2021 ◽  
pp. 211-253
Author(s):  
Moataz H. Emam
Keyword(s):  
Black Hole ◽  
Vector Fields ◽  
Killing Vector ◽  
Schwarzschild Black Hole ◽  
Curved Spacetime ◽  
Killing Vector Fields ◽  
Event Horizons ◽  
Free Particles ◽  
Generally Covariant

We discuss mechanics in curved spacetime backgrounds, gravitational time dilation, the motion of free particles, geodesics. We use the Schwarzschild metric as a case study and solve for motion along radial and orbital geodesics. This includes the strange behaviour around the event horizons of a Schwarzschild black hole. Isometries and Killing vector fields are explained and applied. Finally a brief presentation of generally covariant electrodynamics is given.

scholarly journals Schrödinger equation in a general curved spacetime geometry

2022 ◽  
Author(s):  
Qasem Exirifard ◽  
Ebrahim Karimi
Keyword(s):  
Black Hole ◽  
Schrödinger Equation ◽  
Schrodinger Equation ◽  
Relativistic Quantum ◽  
Quantum Field ◽  
Relativistic Quantum Field Theory ◽  
Schwarzschild Black Hole ◽  
Curved Spacetime ◽  
Spacetime Geometry ◽  
Energy Physics

In this paper, we consider relativistic quantum field theory in the presence of an external electric potential in a general curved spacetime geometry. We utilize Fermi coordinates adapted to the time-like geodesic to describe the low-energy physics in the laboratory and calculate the leading correction due to the curvature of the spacetime geometry to the Schrödinger equation. We then compute the nonvanishing probability of excitation for a hydrogen atom that falls in or is scattered by a general Schwarzschild black hole. The photon emitted from the excited state by spontaneous emission extracts energy from the black hole, increases the decay rate of the black hole and adds to the information paradox.

scholarly journals Note on uncertainty relations in doubly special relativity and gravity’s rainbow

2015 ◽  
Vol 30 (33) ◽  
pp. 1550178 ◽  
Author(s):  
Edwin J. Son ◽  
Wontae Kim
Keyword(s):  
Black Hole ◽  
Special Relativity ◽  
Hawking Temperature ◽  
Uncertainty Relations ◽  
Schwarzschild Black Hole ◽  
Commutation Relations ◽  
Gravity’S Rainbow ◽  
Gravity's Rainbow ◽  
Doubly Special Relativity

We present commutation relations depending on the rainbow functions which are slightly different from the well-known results. However, the advantage of these new commutation relations are compatible with the calculation of the Hawking temperature in the rainbow Schwarzschild black hole.

GRAVITATIONAL THERMODYNAMICS AND THE WHEELER–DEWITT EQUATION

2011 ◽  
Vol 20 (01) ◽  
pp. 23-42 ◽  
Author(s):  
M. D. POLLOCK
Keyword(s):  
Black Hole ◽  
Wave Function ◽  
Boundary Conditions ◽  
Cosmological Constant ◽  
Apparent Horizon ◽  
De Sitter Space ◽  
Hawking Temperature ◽  
De Sitter ◽  
Schwarzschild Black Hole ◽  
Gravitational Thermodynamics

In a previous paper, we have derived the Hawking temperature T H = 1/8πM for a Schwarzschild black hole of mass M, starting from the Wheeler–DeWitt for the wave function Ψ on the apparent horizon, due to Tomimatsu. Here we discuss the derivation of this result in greater detail, with particular regard to the Euclideanization procedure involved and the boundary conditions on the horizon. Further, analysis of the de Sitter space-time generated by a cosmological constant Λ yields the temperature [Formula: see text] found by Gibbons and Hawking, which thus vindicates the method. The emission of radiation occurs with preservation of unitarity, and hence entropy, which is substantiated by a global thermodynamical argument in the case of the black hole.

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