scholarly journals Critical behaviors of 3D black holes with a scalar hair

2015 ◽  
Vol 12 (02) ◽  
pp. 1550017 ◽  
Author(s):  
A. Belhaj ◽  
M. Chabab ◽  
H. El Moumni ◽  
K. Masmar ◽  
M. B. Sedra
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Moduli Space ◽  
Three Dimensional ◽  
Perfect Gas ◽  
Btz Black Hole ◽  
Scalar Hair ◽  
Two Parameters ◽  
Thermodynamic Pressure

The principal focus of the present work concerns the critical behaviors of a class of three-dimensional (3D) black holes with a scalar field hair. Since the cosmological constant is viewed as a thermodynamic pressure and its conjugate quantity as a volume, we examine such properties in terms of two parameters B and a. The latters are related to the scalar field and the angular momentum, respectively. In particular, we give the equation of state predicting a critical universal number depending on the (B, a) moduli space. In the vanishing limit of the B parameter, we recover the usual perfect gas behavior appearing in the case of the non-rotating BTZ black hole. We point out that in a generic region of the (B, a) moduli space, the model behaves like a Van der Waals system.

scholarly journals A new spin on black hole hair

2014 ◽  
Vol 23 (12) ◽  
pp. 1442014 ◽  
Author(s):  
Carlos A. R. Herdeiro ◽  
Eugen Radu
Keyword(s):  
Black Holes ◽  
General Relativity ◽  
Black Hole ◽  
Scalar Field ◽  
Massive Scalar ◽  
Massive Scalar Field ◽  
Hairy Black Holes ◽  
Scalar Hair

We show that scalar hair can be added to rotating, vacuum black holes (BHs) of general relativity. These hairy black holes (HBHs) clarify a lingering question concerning gravitational solitons: Whether a BH can be added at the centre of a boson star (BS), as it typically can for other solitons. We argue that it can, but only if it is spinning. The existence of such HBHs is related to the Kerr superradiant instability triggered by a massive scalar field. This connection leads to the following conjecture: a (hairless) BH, which is afflicted by the superradiant instability of a given field, must allow hairy generalizations with that field.

scholarly journals UNITARITY ISSUE IN BTZ BLACK HOLES

2006 ◽  
Vol 21 (22) ◽  
pp. 1737-1748 ◽  
Author(s):  
Y. S. MYUNG ◽  
H. W. LEE
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Wave Equation ◽  
Three Dimensional ◽  
Btz Black Hole ◽  
Unitary Evolution ◽  
Potential Analysis ◽  
Black Hole Spacetimes ◽  
Ads Spacetime ◽  
Extremal Black Holes

We study the wave equation for a massive scalar in three-dimensional AdS-black hole spacetimes to understand the unitarity issues in a semiclassical way. Here we introduce four interesting spacetimes: the non-rotating BTZ black hole (NBTZ), pure AdS spacetime (PADS), massless BTZ black hole (MBTZ), and extremal BTZ black hole (EBTZ). Our method is based on the potential analysis and solving the wave equation to find the condition for the frequency ω exactly. In the NBTZ case, one finds the quasinormal (complex and discrete) modes which signals for a non-unitary evolution. Real and discrete modes are found for the PADS case, which means that it is unitary obviously. On the other hand, we find real and continuous modes for the two extremal black holes of MBTZ and EBTZ. It suggests that these could be candidates for the unitary system.

THOUGHTS ON THE AREA THEOREM

2009 ◽  
Vol 24 (16n17) ◽  
pp. 3111-3135 ◽  
Author(s):  
MU-IN PARK
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Three Dimensional ◽  
Kerr Black Hole ◽  
Second Law Of Thermodynamics ◽  
Positive Energy ◽  
Btz Black Hole ◽  
Area Theorem ◽  
Four Dimensions ◽  
Higher Derivative

Hawking's area theorem can be understood from a quasistationary process in which a black hole accretes positive energy matter, independent of the details of the gravity action. I use this process to study the dynamics of the inner as well as the outer horizons for various black holes which include the recently discovered exotic black holes and three-dimensional black holes in higher derivative gravities as well as the usual Banados–Teitelboim–Zanelli (BTZ) black hole and the Kerr black hole in four dimensions. I find that the area for the inner horizon "can decrease," rather than increase, with the quasistationary process. However, I find that the area for the outer horizon "never decrease" such as the usual area theorem still works in our examples, though this is quite nontrivial in general. I also find that the recently proposed new entropy formulae for the above mentioned, recently discovered black holes satisfy the second law of thermodynamics.

SCALAR HAIR FOR AN AdS BLACK HOLE

2006 ◽  
Vol 21 (38) ◽  
pp. 2893-2902
Author(s):  
P. I. KURIAKOSE ◽  
V. C. KURIAKOSE
Keyword(s):  
Black Hole ◽  
Scalar Field ◽  
Naked Singularity ◽  
Massive Scalar ◽  
Btz Black Hole ◽  
Massive Scalar Field ◽  
Stability Of Solution ◽  
Scalar Hair ◽  
The Stability ◽  
Double Well Potential

A nontrivial scalar solution, whose source is a massive scalar field with a double-well potential, for a non-rotating Bananas–Teitelboim–Zanelli (BTZ) black hole is obtained with a condition [Formula: see text], where μ is the mass of scalar field and [Formula: see text] the cosmological constant. The stability of solution is also studied. The mass of black hole with a scalar hair is greater than the black hole without hair. The scalar solution proposes a regular horizon which hides the naked singularity.

scholarly journals Interior of the horizon of the Bañados-Teitelboim-Zanelli black hole

2020 ◽  
Vol 2020 (12) ◽  
Author(s):  
Ryuichi Nakayama ◽  
Kenji Shiohara
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Normal Modes ◽  
Integral Form ◽  
Matching Condition ◽  
Btz Black Hole ◽  
Mode Expansion ◽  
Higher Dimensional ◽  
Appropriate Prescription

Abstract A quantum scalar field inside the horizon of the non-rotating BTZ black hole is studied. Not only the near-horizon modes but also the normal modes deep inside the horizon are obtained. It is shown that the matching condition for the normal modes of a scalar field at the horizon does not uniquely determine the normal-mode expansion of a scalar field inside the horizon. By choosing a certain appropriate prescription for removing this ambiguity, an integral form of a new scalar propagator for points on both sides of the horizon are obtained. A similar problem may arise in higher-dimensional black holes.

scholarly journals Thermodynamics of de Sitter black holes with conformally coupled scalar fields

2021 ◽  
Vol 2021 (2) ◽  
Author(s):  
Fil Simovic ◽  
Danny Fusco ◽  
Robert B. Mann
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Phase Transitions ◽  
Scalar Field ◽  
Scalar Fields ◽  
De Sitter ◽  
Finite Radius ◽  
Extended Phase ◽  
Black Hole Spacetime ◽  
Thermodynamic Pressure

Abstract We investigate the thermodynamic properties of 3+1 dimensional black holes in asymptotically de Sitter spacetimes, conformally coupled to a real scalar field. We use a Euclidean action approach, where boundary value data is specified at a finite radius ‘cavity’ outside the black hole, working in the extended phase space where the cosmological constant is treated as a thermodynamic pressure. We examine the phase structure of these black holes through their free energy. For the MTZ subclass of solutions, we find Hawking-Page-like phase transitions from a black hole spacetime to thermal de Sitter with a scalar field. In the more general case, Hawking-Page-like phase transitions are also present, whose existence depends further on a particular cosmic censorship bound.

scholarly journals Throat quantization of the Schwarzschild-Tangherlini(-AdS) black hole

2018 ◽  
Vol 168 ◽  
pp. 03009
Author(s):  
Hideki Maeda
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Three Dimensional ◽  
Large Mass ◽  
Wkb Approximation ◽  
Btz Black Hole ◽  
Asymptotically Flat ◽  
Ads Black Holes ◽  
Arbitrary Dimensions

By the throat quantization pioneered by Louko and Mäkelä, we derive the mass and area/entropy spectra for the Schwarzschild-Tangherlini-type asymptotically flat or AdS vacuum black hole in arbitrary dimensions. Using the WKB approximation for black holes with large mass, we show that area/entropy is equally spaced for asymptotically flat black holes, while mass is equally spaced for asymptotically AdS black holes. Exact spectra can be obtained for toroidal AdS black holes in arbitrary dimensions including the three-dimensional BTZ black hole.

scholarly journals Inside an asymptotically flat hairy black hole

2021 ◽  
Vol 2021 (12) ◽  
Author(s):  
Óscar J. C. Dias ◽  
Gary T. Horowitz ◽  
Jorge E. Santos
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Holographic Superconductor ◽  
Charged Scalar ◽  
General Argument ◽  
Asymptotically Flat ◽  
Charged Black Holes ◽  
Scalar Hair ◽  
Hairy Black Hole

Abstract We study the interior of a recently constructed family of asymptotically flat, charged black holes that develop (charged) scalar hair as one increases their charge at fixed mass. Inside the horizon, these black holes resemble the interior of a holographic superconductor. There are analogs of the Josephson oscillations of the scalar field, and the final Kasner singularity depends very sensitively on the black hole parameters near the onset of the instability. In an appendix, we give a general argument that Cauchy horizons cannot exist in a large class of stationary black holes with scalar hair.

scholarly journals Spinning boson stars and hairy black holes with nonminimal coupling

2018 ◽  
Vol 27 (11) ◽  
pp. 1843009 ◽  
Author(s):  
Carlos A. R. Herdeiro ◽  
Eugen Radu
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Coupling Parameter ◽  
Nonminimal Coupling ◽  
Boson Stars ◽  
Hairy Black Holes ◽  
Black Hole Solutions ◽  
Hairy Black Hole ◽  
Coupled Theory

We obtain spinning boson star solutions and hairy black holes with synchronized hair in the Einstein–Klein–Gordon model, wherein the scalar field is massive, complex and with a nonminimal coupling to the Ricci scalar. The existence of these hairy black holes in this model provides yet another manifestation of the universality of the synchronization mechanism to endow spinning black holes with hair. We study the variation of the physical properties of the boson stars and hairy black holes with the coupling parameter between the scalar field and the curvature, showing that they are, qualitatively, identical to those in the minimally coupled case. By discussing the conformal transformation to the Einstein frame, we argue that the solutions herein provide new rotating boson star and hairy black hole solutions in the minimally coupled theory, with a particular potential, and that no spherically symmetric hairy black hole solutions exist in the nonminimally coupled theory, under a condition of conformal regularity.

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