scholarly journals Cold plasma dispersion relations in the vicinity of a Schwarzschild black hole horizon

2007 ◽  
Vol 39 (9) ◽  
pp. 1437-1465 ◽  
Author(s):  
M. Sharif ◽  
Umber Sheikh
Keyword(s):  
Black Hole ◽  
Cold Plasma ◽  
Dispersion Relations ◽  
Black Hole Horizon ◽  
Schwarzschild Black Hole ◽  
Plasma Dispersion

scholarly journals Moving Schwarzschild black hole and modified dispersion relations

2015 ◽  
Vol 749 ◽  
pp. 431-436 ◽  
Author(s):  
Cristian Barrera Hinojosa ◽  
Justo López-Sarrión
Keyword(s):  
Black Hole ◽  
Dispersion Relations ◽  
Schwarzschild Black Hole ◽  
Modified Dispersion Relations

Black Hole Spectroscopy in the Isotropic Coordinate

2013 ◽  
Vol 785-786 ◽  
pp. 1348-1352
Author(s):  
Bing Bing Chen ◽  
Wei Ren ◽  
Jian Tang
Keyword(s):  
Black Hole ◽  
Black Hole Horizon ◽  
Schwarzschild Black Hole ◽  
Horizon Area ◽  
Oscillation Velocity

In this paper, the black hole spectroscopy is intriguingly described in the isotropic coordinate by combining the black hole property of adiabaticity and the oscillation velocity of the black hole horizon. The result shows that the horizon area of a Schwarzschild black hole is quantized independent of the choice of coordinates, with an equally spaced spectroscopy always given by .

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.

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