scholarly journals Second-order quasinormal mode of the Schwarzschild black hole

2007 ◽  
Vol 76 (8) ◽  
Author(s):  
Hiroyuki Nakano ◽  
Kunihito Ioka
Keyword(s):  
Black Hole ◽  
Second Order ◽  
Quasinormal Mode ◽  
Schwarzschild Black Hole

scholarly journals THE EVENT HORIZON OF THE SCHWARZSCHILD BLACK HOLE IN NONCOMMUTATIVE SPACES

2006 ◽  
Vol 15 (07) ◽  
pp. 1113-1117 ◽  
Author(s):  
FOROUGH NASSERI
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Lower Limit ◽  
Second Order ◽  
Schwarzschild Black Hole ◽  
Perturbative Calculations ◽  
First Order ◽  
Noncommutative Spaces

The event horizon of the Schwarzschild black hole is obtained in noncommutative spaces up to the second order of perturbative calculations. Because this type of black hole is non-rotating, to the first order there is no effect on the event horizon due to the noncommutativity of space. A lower limit for the noncommutativity parameter is also obtained. As a result, the event horizon in noncommutative spaces is less than the event horizon in commutative spaces.

scholarly journals ASYMPTOTIC QUASINORMAL MODES OF d-DIMENSIONAL SCHWARZSCHILD BLACK HOLE WITH GAUSS–BONNET CORRECTION

2006 ◽  
Vol 21 (17) ◽  
pp. 3565-3574 ◽  
Author(s):  
SAYAN K. CHAKRABARTI ◽  
KUMAR S. GUPTA
Keyword(s):  
Black Hole ◽  
Quasinormal Modes ◽  
Quasinormal Mode ◽  
Minimum Length ◽  
Length Scale ◽  
Schwarzschild Black Hole ◽  
Analytic Expression ◽  
Models Of Gravity ◽  
Minimum Length Scale ◽  
Bonnet Term

We obtain an analytic expression for the highly damped asymptotic quasinormal mode frequencies of the (d ≥ 5)-dimensional Schwarzschild black hole modified by the Gauss–Bonnet term, which appears in string derived models of gravity. The analytic expression is obtained under the string inspired assumption that there exists a minimum length scale in the system and in the limit when the coupling in front of the Gauss–Bonnet term in the action is small. Although there are several similarities of this geometry with that of the Schwarzschild black hole, the asymptotic quasinormal mode frequencies are quite different. In particular, the real part of the asymptotic quasinormal frequencies for this class of single horizon black holes is not proportional to log (3).

scholarly journals Second Order Perturbations of a Schwarzschild Black Hole: Inclusion of Odd Parity Perturbations

2000 ◽  
Vol 32 (10) ◽  
pp. 2021-2042 ◽  
Author(s):  
Carlos O. Nicasio ◽  
Reinaldo Gleiser ◽  
Jorge Pullin
Keyword(s):  
Black Hole ◽  
Second Order ◽  
Schwarzschild Black Hole

scholarly journals Accretion-induced quasinormal mode excitation of a Schwarzschild black hole

2007 ◽  
Vol 75 (4) ◽  
Author(s):  
Alessandro Nagar ◽  
Olindo Zanotti ◽  
José A. Font ◽  
Luciano Rezzolla
Keyword(s):  
Black Hole ◽  
Quasinormal Mode ◽  
Schwarzschild Black Hole ◽  
Mode Excitation

scholarly journals Second-order perturbations of a Schwarzschild black hole

1996 ◽  
Vol 13 (10) ◽  
pp. L117-L124 ◽  
Author(s):  
Reinaldo J Gleiser ◽  
Carlos O Nicasio ◽  
Richard H Price ◽  
Jorge Pullin
Keyword(s):  
Black Hole ◽  
Second Order ◽  
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.

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