scholarly journals Canonical quantization and the statistical entropy of the Schwarzschild black hole

2000 ◽  
Vol 61 (6) ◽  
Author(s):  
Cenalo Vaz
Keyword(s):  
Black Hole ◽  
Canonical Quantization ◽  
Statistical Entropy ◽  
Schwarzschild Black Hole

scholarly journals BOUND OF NONCOMMUTATIVITY PARAMETER BASED ON BLACK HOLE ENTROPY

2010 ◽  
Vol 25 (38) ◽  
pp. 3213-3218 ◽  
Author(s):  
WONTAE KIM ◽  
DAEHO LEE
Keyword(s):  
Black Hole ◽  
Gauge Group ◽  
Black Hole Entropy ◽  
Brick Wall ◽  
Statistical Entropy ◽  
Schwarzschild Black Hole ◽  
Cutoff Parameter ◽  
Entropy Satisfying ◽  
Area Law ◽  
Wall Method

We study the bound of the noncommutativity parameter in the noncommutative Schwarzschild black hole which is a solution of the noncommutative ISO(3, 1) Poincaré gauge group. The statistical entropy satisfying the area law in the brick wall method yields a cutoff relation which depends on the noncommutativity parameter. Requiring both the cutoff parameter and the noncommutativity parameter to be real, the noncommutativity parameter can be shown to be bounded as Θ > 8.4 × 10-2lp.

scholarly journals STATISTICAL ENTROPY OF THE SCHWARZSCHILD BLACK HOLE

2006 ◽  
Vol 21 (24) ◽  
pp. 1879-1887 ◽  
Author(s):  
MARIANO CADONI
Keyword(s):  
Black Hole ◽  
Central Charge ◽  
Virasoro Algebra ◽  
Symmetry Algebra ◽  
Energy Tensor ◽  
De Sitter ◽  
Statistical Entropy ◽  
Schwarzschild Black Hole ◽  
Null Infinity ◽  
Weyl Invariance

We derive the statistical entropy of the Schwarzschild black hole by considering the asymptotic symmetry algebra near the [Formula: see text] boundary of the spacetime at past null infinity. Using a two-dimensional description and the Weyl invariance of black hole thermodynamics this symmetry algebra can be mapped into the Virasoro algebra generating asymptotic symmetries of anti-de Sitter spacetime. Using Lagrangian methods we identify the stress–energy tensor of the boundary conformal field theory and calculate the central charge of the Virasoro algebra. The Bekenstein–Hawking result for the black hole entropy is regained using Cardy's formula. Our result strongly supports a nonlocal realization of the holographic principle.

scholarly journals Statistical entropy of the four dimensional Schwarzschild black hole

1998 ◽  
Vol 426 (3-4) ◽  
pp. 275-281 ◽  
Author(s):  
R. Argurio ◽  
F. Englert ◽  
L. Houart
Keyword(s):  
Black Hole ◽  
Statistical Entropy ◽  
Schwarzschild Black Hole

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.

scholarly journals Black hole S-matrix for a scalar field

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Panos Betzios ◽  
Nava Gaddam ◽  
Olga Papadoulaki
Keyword(s):  
Black Hole ◽  
Normal Modes ◽  
Massless Scalar ◽  
Scattering Process ◽  
Schwarzschild Black Hole ◽  
Asymptotically Flat ◽  
Scalar Particles ◽  
Black Hole Background ◽  
S Matrix ◽  
Do So

Abstract We describe a unitary scattering process, as observed from spatial infinity, of massless scalar particles on an asymptotically flat Schwarzschild black hole background. In order to do so, we split the problem in two different regimes governing the dynamics of the scattering process. The first describes the evolution of the modes in the region away from the horizon and can be analysed in terms of the effective Regge-Wheeler potential. In the near horizon region, where the Regge-Wheeler potential becomes insignificant, the WKB geometric optics approximation of Hawking’s is replaced by the near-horizon gravitational scattering matrix that captures non-perturbative soft graviton exchanges near the horizon. We perform an appropriate matching for the scattering solutions of these two dynamical problems and compute the resulting Bogoliubov relations, that combines both dynamics. This allows us to formulate an S-matrix for the scattering process that is manifestly unitary. We discuss the analogue of the (quasi)-normal modes in this setup and the emergence of gravitational echoes that follow an original burst of radiation as the excited black hole relaxes to equilibrium.

Sign in / Sign up

Export Citation Format

Share Document