scholarly journals Object picture of scalar field perturbation on Kerr black hole in scalar-Einstein-Gauss-Bonnet theory

2020 ◽  
Vol 102 (12) ◽  
Author(s):  
Shao-Jun Zhang ◽  
Bin Wang ◽  
Anzhong Wang ◽  
Joel F. Saavedra
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Kerr Black Hole ◽  
Field Perturbation ◽  
Object Picture

scholarly journals Massive scalar field perturbation on Kerr black holes in dynamical Chern–Simons gravity

2021 ◽  
Vol 81 (5) ◽  
Author(s):  
Shao-Jun Zhang
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Massive Scalar ◽  
Coupling Constant ◽  
Field Mass ◽  
Field Perturbation ◽  
Massive Scalar Field ◽  
Kerr Black Holes ◽  
Chern Simons

AbstractWe study massive scalar field perturbation on Kerr black holes in dynamical Chern–Simons gravity by performing a $$(2+1)$$ ( 2 + 1 ) -dimensional simulation. Object pictures of the wave dynamics in time domain are obtained. The tachyonic instability is found to always occur for any nonzero black hole spin and any scalar field mass as long as the coupling constant exceeds a critical value. The presence of the mass term suppresses or even quench the instability. The quantitative dependence of the onset of the tachyonic instability on the coupling constant, the scalar field mass and the black hole spin is given numerically.

scholarly journals The limit y of the incident particle under the superradiance of Kerr black hole

2021 ◽  
Author(s):  
Wen-Xiang Chen
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Kerr Black Hole ◽  
Weak Field ◽  
Incident Particle ◽  
Field Coupling ◽  
Field System ◽  
Field Behavior

It is important to emphasize that as the reference has proved well, the critical storage line of black hole field system is universal, that is, different scalar field coupling functions with the same weak field behavior are $\{C(\phi) \} , C (\phi) =1+\alpha\phi ^{2} + o(\phi ^{4})$, and have the same function behavior $\alpha=\alpha (\mu); a / M) $. The purpose of this paper is to find out the limit $y$ of the incident particle under the superradiance of the preset boundary (${\mu} = {y}{\omega}$).

scholarly journals On the stability of the scalar field in the gravitational field of a rotating (Kerr-) black hole

2010 ◽  
Author(s):  
Reinhard Horst Beyer ◽  
H. A. Morales-Tecotl ◽  
L. A. Urena-Lopez ◽  
R. Linares-Romero ◽  
H. H. Garcia-Compean
Keyword(s):  
Black Hole ◽  
Gravitational Field ◽  
Scalar Field ◽  
Kerr Black Hole ◽  
The Stability

Thermal Casimir effect in the Kerr spacetime with quintessence

2019 ◽  
Vol 34 (16) ◽  
pp. 1950125
Author(s):  
V. B. Bezerra ◽  
J. M. Toledo
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Equatorial Plane ◽  
Casimir Effect ◽  
Kerr Black Hole ◽  
Casimir Energy ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Kerr Spacetime

We calculate thermal corrections to the Casimir energy of a massless scalar field in the Kerr black hole surrounded by quintessence, taking into account the metrics derived by Ghosh [S. G. Ghosh, Eur. Phys. J. C 76, 222 (2016)] and Toshmatov et al. [B. Toshmatov, Z. Stuchlík and B. Ahmedov, Eur. Phys. J. Plus 132, 98 (2017)]. We compare both results and show that they are almost the same, except very close to the horizons. At [Formula: see text], equatorial plane, the results are the same, as should be expected, due to the fact that the metrics coincide in this region.

scholarly journals Comments on “Casimir effect in the Kerr spacetime with quintessence”

2017 ◽  
Vol 32 (21) ◽  
pp. 1775001 ◽  
Author(s):  
Bobir Toshmatov ◽  
Zdeněk Stuchlík ◽  
Bobomurat Ahmedov
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Casimir Effect ◽  
Kerr Black Hole ◽  
Casimir Energy ◽  
Massless Scalar ◽  
Massless Scalar Field ◽  
Kerr Spacetime ◽  
The Difference

This comment is devoted to the recalculation of the Casimir energy of a massless scalar field in the Kerr black hole surrounded by quintessence derived in [B. Toshmatov, Z. Stuchlík and B. Ahmedov, Eur. Phys. J. Plus 132, 98 (2017)] and its comparison with the results recently obtained in [V. B. Bezerra, M. S. Cunha, L. F. F. Freitas and C. R. Muniz, Mod. Phys. Lett. A 32, 1750005 (2017)] in the spacetime [S. G. Ghosh, Eur. Phys. J. C 76, 222 (2016)]. We have shown that in the more realistic spacetime which does not have the failures illustrated here, the Casimir energy is significantly bigger than that derived in [V. B. Bezerra, M. S. Cunha, L. F. F. Freitas and C. R. Muniz, Mod. Phys. Lett. A 32, 1750005 (2017)], and the difference becomes crucial especially in the regions of near horizons of the spacetime.

scholarly journals Observing the inhomogeneity in the holographic models of superconductors

2014 ◽  
Vol 29 (14) ◽  
pp. 1450070 ◽  
Author(s):  
Xiao-Mei Kuang ◽  
Bin Wang ◽  
Xian-Hui Ge
Keyword(s):  
Black Hole ◽  
Critical Temperature ◽  
Scalar Field ◽  
Chemical Potential ◽  
Normal Phase ◽  
Field Perturbation ◽  
Holographic Superconductors ◽  
Gravity Duals

We study the gravity duals of striped holographic superconductors in the AdS black hole and AdS soliton backgrounds. We show the dependences of the condensation and the critical temperature/critical chemical potential on the inhomogeneity in these two different spacetimes. By exploring the dynamics of the normal phase through the scalar field perturbation, we argue that the pair susceptibility and the conductivity can be possible phenomenological indications to disclose the property of inhomogeneity.

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 Scalar field effects on the orbit of S2 star

2019 ◽  
Vol 489 (4) ◽  
pp. 4606-4621 ◽  
Author(s):  
◽  
A Amorim ◽  
M Bauböck ◽  
M Benisty ◽  
J-P Berger ◽  
...  
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Scalar Field ◽  
Coupling Parameter ◽  
Kerr Black Hole ◽  
Compact Object ◽  
Relative Mass ◽  
Exact Nature ◽  
Main Effect ◽  
Open Debate

ABSTRACT Precise measurements of the S-stars orbiting SgrA* have set strong constraints on the nature of the compact object at the centre of the Milky Way. The presence of a black hole in that region is well established, but its neighbouring environment is still an open debate. In that respect, the existence of dark matter in that central region may be detectable due to its strong signatures on the orbits of stars: the main effect is a Newtonian precession which will affect the overall pericentre shift of S2, the latter being a target measurement of the GRAVITY instrument. The exact nature of this dark matter (e.g. stellar dark remnants or diffuse dark matter) is unknown. This article assumes it to be a scalar field of toroidal distribution, associated with ultralight dark matter particles, surrounding the Kerr black hole. Such a field is a form of ‘hair’ expected in the context of superradiance, a mechanism that extracts rotational energy from the black hole. Orbital signatures for the S2 star are computed and shown to be detectable by GRAVITY. The scalar field can be constrained because the variation of orbital elements depends both on the relative mass of the scalar field to the black hole and on the field mass coupling parameter.

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