scholarly journals Scalar quasinormal modes of the near extremal Reissner-Nordström black hole in NC space-time

2019 ◽  
Vol 17 (1, spec.issue) ◽  
pp. 43-51
Author(s):  
Marija Dimitrijevic-Ciric ◽  
Nikola Konjik ◽  
Andjelo Samsarov
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Gauge Symmetry ◽  
Symmetry Group ◽  
Quasinormal Modes ◽  
Space Time ◽  
Complex Scalar ◽  
Mode Spectrum ◽  
Extremal Limit ◽  
Complex Scalar Field

A way to search for a signal of space-time noncommutativity is to study a quasinormal mode spectrum of the Reissner-Nordstr?m black hole in the presence of noncommutativity. In this paper, we chose a particular NC deformation defined by the angular twist. We investigate a noncommutative (NC) deformation of a complex scalar field, minimally coupled with a classical (commutative) near extremal Reissner-Nordstr?m background. The theory is manifestly invariant under the deformed U(1)* gauge symmetry group. Using the EOM for the NC complex scalar field in RN background, the QNM spectrum is calculated for a particular range of parameters coresponding to the near extremal limit.

scholarly journals DECAY OF SPIN-1/2 FIELD AROUND REISSNER–NORDSTROM BLACK HOLE

2004 ◽  
Vol 13 (06) ◽  
pp. 1105-1118 ◽  
Author(s):  
WEI ZHOU ◽  
JIAN-YANG ZHU
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Quantum Number ◽  
Turning Point ◽  
Quasinormal Modes ◽  
Astronomical Observation ◽  
Dirac Field ◽  
Neutrino Field ◽  
Extremal Limit ◽  
Field Decay

To find what influence the charge of the black hole Q will bring to the evolution of the quasinormal modes, we calculate the quasinormal frequencies of the neutrino field (charge e=0) perturbations and those of the massless Dirac field (e≠0) perturbations in the RN metric. The influences of Q, e, the momentum quantum number l, and the mode number n are discussed. Among the conclusions, the most important one is that, at the stage of quasinormal ringing, when the black hole and the field have the same kind of charge (eQ>0), the quasinormal modes of the massless charged Dirac field decay faster than those of the neutral ones, and when eQ<0, the massless charged Dirac field decays slower, which may be helpful in the astronomical observation. In addition, we compare the influence from the charge of the black hole to the spin 1/2 field and scalar field perturbations including the extremal limit (M=Q) and find a turning point of Q exists in both cases. The explanation of this fact is unclear with some suggestions that may be helpful are given.

scholarly journals DIRAC MONOPOLES AND HAWKING RADIATION IN KOTTLER SPACETIME

2002 ◽  
Vol 17 (32) ◽  
pp. 4947-4957
Author(s):  
A. A. BYTSENKO ◽  
YU. P. GONCHAROV
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Energy Density ◽  
Hawking Radiation ◽  
Natural Extension ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Radiation Process ◽  
Complex Scalar Field ◽  
The Given

The natural extension of Schwarzschild metric to the case of nonzero cosmological constant Λ known as the Kottler metric is considered and it is discussed under what circumstances the given metric could describe the Schwarzschild black hole immersed in a medium with nonzero energy density. Under the latter situation such an object might carry topologically inequivalent configurations of various fields. The given possibility is analyzed for complex scalar field and it is shown that the mentioned configurations might be tied with natural presence of Dirac monopoles on black hole under consideration. In turn, this could markedly modify the Hawking radiation process.

scholarly journals Complex Scalar Field Reheating and Primordial Black Hole production

2021 ◽  
Vol 2021 (07) ◽  
pp. 001
Author(s):  
Karim Carrion ◽  
Juan Carlos Hidalgo ◽  
Ariadna Montiel ◽  
Luis E. Padilla
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Primordial Black Hole ◽  
Complex Scalar ◽  
Complex Scalar Field

scholarly journals On the pattern of black hole information release

2014 ◽  
Vol 29 (09) ◽  
pp. 1450047 ◽  
Author(s):  
I. Y. Park ◽  
F. James
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Scattering Amplitudes ◽  
Cross Section ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Mass Growth ◽  
Complex Scalar Field ◽  
Black Hole Information ◽  
Flux Loss

We propose a step towards a resolution to black hole information paradox by analyzing scattering amplitudes of a complex scalar field around a Schwarzschild black hole. The scattering cross-section reveals much information on the incoming state but exhibits flux loss at the same time. The flux loss should be temporary, and indicate mass growth of the black hole. The black hole should Hawking-radiate subsequently, thereby, compensating for the flux loss. By examining the purity issue, we comment on the possibility that information bleaching may be the key to the paradox.

INCREASE OF HAWKING RADIATION FROM BLACK HOLES BY DIRAC MONOPOLES

1996 ◽  
Vol 05 (04) ◽  
pp. 419-432 ◽  
Author(s):  
YU. P. GONCHAROV ◽  
N.E. FIRSOVA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Schwarzschild Black Hole ◽  
Complex Scalar ◽  
Total Luminosity ◽  
Complex Scalar Field

We study a mechanism of increasing Hawking radiation from a black hole by using the example of twisted topologically inequivalent configurations (TICs) of a complex scalar field on the Schwarzschild black hole. Physically this increase is tied with the natural presence of Dirac monopoles on black holes. We satisfy both analytical and numerical considerations and find that twisted TICs give the contribution of order 17% to the total luminosity (summed up over all the TICs) of a black hole.

scholarly journals ON GENERALIZED MONOPOLE SPHERICAL HARMONICS AND THE WAVE EQUATION OF A CHARGED MASSIVE KERR BLACK HOLE

2010 ◽  
Vol 25 (38) ◽  
pp. 3191-3200
Author(s):  
SHABNAM BEHESHTI ◽  
FLOYD L. WILLIAMS
Keyword(s):  
Black Hole ◽  
Wave Equation ◽  
Scalar Field ◽  
Spherical Harmonics ◽  
Spherical Harmonic ◽  
Kerr Black Hole ◽  
Complex Scalar ◽  
Linearly Independent ◽  
Complex Scalar Field

We find linearly independent solutions of the Goncharov–Firsova equation in the case of a massive complex scalar field on a Kerr black hole. The solutions generalize, in some sense, the classical monopole spherical harmonic solutions previously studied in the massless cases.

scholarly journals Critical exponents and stability at the black hole threshold for a complex scalar field

1995 ◽  
Vol 52 (10) ◽  
pp. 5850-5856 ◽  
Author(s):  
Eric W. Hirschmann ◽  
Douglas M. Eardley
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Critical Exponents ◽  
Complex Scalar ◽  
Complex Scalar Field

scholarly journals Wave Function for the Reissner–Nordström Black Hole

1997 ◽  
Vol 12 (20) ◽  
pp. 1491-1505 ◽  
Author(s):  
P. V. Moniz
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Function ◽  
Scalar Field ◽  
Hawking Radiation ◽  
Apparent Horizon ◽  
Complex Scalar ◽  
Charge Rate ◽  
Quantum Behavior ◽  
Complex Scalar Field

We study the quantum behavior of Reissner–Nordström (RN) black holes interacting with a complex scalar field. A Maxwell field is also present. Our analysis is based on M. Pollock's1 method and is characterized by solving a Wheeler–DeWitt equation in the proximity of an apparent horizon of the RN space–time. Subsequently, we obtain a wave function Ψ RN [M,Q] representing the RN black hole when its charge, |Q|, is small in comparison with its mass, M. We then compare quantum-mechanically the cases of (i) Q=0 and (ii) M≥|Q|≠0. A special emphasis is given to the evolution of the mass-charge rate affected by Hawking radiation.

scholarly journals Stability analysis of a charged black hole with a nonlinear complex scalar field

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
Zhan-Feng Mai ◽  
Run-Qiu Yang
Keyword(s):  
Black Hole ◽  
Stability Analysis ◽  
Scalar Field ◽  
Charged Black Hole ◽  
Complex Scalar ◽  
Complex Scalar Field

scholarly journals Effects of oscillating spacetime metric background on a complex scalar field and formation of topological vortices

2021 ◽  
Vol 103 (11) ◽  
Author(s):  
Shreyansh S. Dave ◽  
Sanatan Digal
Keyword(s):  
Scalar Field ◽  
Complex Scalar ◽  
Complex Scalar Field ◽  
Spacetime Metric
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