scholarly journals THERMODYNAMICS OF NONSPHERICAL BLACK HOLES FROM LIOUVILLE THEORY

2012 ◽  
Vol 27 (20) ◽  
pp. 1250111 ◽  
Author(s):  
FANG-FANG YUAN ◽  
YONG-CHANG HUANG
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Central Charge ◽  
Black Hole Entropy ◽  
Liouville Theory ◽  
Two Dimensional ◽  
Hamiltonian Approach ◽  
Black Rings ◽  
Dimensional Black Hole ◽  
Black Hole Temperature

A Liouville formalism was proposed many years ago to account for the black hole entropy. It was recently updated to connect thermodynamics of general black holes, in particular the Hawking temperature, to two-dimensional Liouville theory. This relies on the dimensional reduction to two-dimensional black hole metric. The relevant dilaton gravity model can be rewritten as a Liouville-like theory. We refine the method and give general formulas for the corresponding scalar and energy–momentum tensors in Liouville theory. This enables us to read off the black hole temperature using a relation which was found about three decades ago. Then the range of application is extended to include nonspherical black holes such as neutral and charged black rings, topological black hole and the case coupled to a scalar field. As for the entropy, following previous authors, we invoke the Lagrangian approach to central charge by Cadoni and then use the Cardy formula. The general relevant parameters are also given. This approach is more advantageous than the usual Hamiltonian approach which was used by the old Liouville formalism for black hole entropy.

scholarly journals Islands in linear dilaton black holes

2021 ◽  
Vol 2021 (3) ◽  
Author(s):  
Georgios K. Karananas ◽  
Alex Kehagias ◽  
John Taskas
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Entanglement Entropy ◽  
Von Neumann Entropy ◽  
Two Dimensional ◽  
Extremal Case ◽  
Von Neumann ◽  
Dimensional Black Hole ◽  
Linear Dilaton ◽  
Linear Dilaton Black Hole

Abstract We derive a novel four-dimensional black hole with planar horizon that asymptotes to the linear dilaton background. The usual growth of its entanglement entropy before Page’s time is established. After that, emergent islands modify to a large extent the entropy, which becomes finite and is saturated by its Bekenstein-Hawking value in accordance with the finiteness of the von Neumann entropy of eternal black holes. We demonstrate that viewed from the string frame, our solution is the two-dimensional Witten black hole with two additional free bosons. We generalize our findings by considering a general class of linear dilaton black hole solutions at a generic point along the σ-model renormalization group (RG) equations. For those, we observe that the entanglement entropy is “running” i.e. it is changing along the RG flow with respect to the two-dimensional worldsheet length scale. At any fixed moment before Page’s time the aforementioned entropy increases towards the infrared (IR) domain, whereas the presence of islands leads the running entropy to decrease towards the IR at later times. Finally, we present a four-dimensional charged black hole that asymptotes to the linear dilaton background as well. We compute the associated entanglement entropy for the extremal case and we find that an island is needed in order for it to follow the Page curve.

Entropy of near-extremal rotating charged black holes in four-dimensional supergravity from AdS2/CFT1 correspondence

2014 ◽  
Vol 29 (13) ◽  
pp. 1450079
Author(s):  
Jun-Jin Peng ◽  
Qing-Ping Hu
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Central Charge ◽  
Conformal Symmetry ◽  
Black Hole Entropy ◽  
Extremal Black Hole ◽  
Charged Black Holes ◽  
Rotating Black Holes ◽  
Cardy Formula ◽  
Asymptotic Symmetries

We study microscopic entropy of the near-extremal rotating black hole in four-dimensional (4D) 𝒩 = 2 supergravity with four charges set pairwise equal from AdS2/CFT1 correspondence. This correspondence is realized in terms of asymptotic symmetries of the AdS2 geometry and a two-dimensional near-horizon effective quantum theory of residual fields from a dimensional reduction proposed by Robinson and Wilczek. We compute the relevant central charge and derive the microscopic entropy of this near-extremal black hole by Cardy formula. Our results can be extended to more general near-extremal rotating black holes in 4D supergravity. They further support the notion that black hole entropy is generally controlled by near-horizon conformal symmetry.

scholarly journals Quantum-Corrected Two-Dimensional Horava-Lifshitz Black Hole Entropy

2016 ◽  
Vol 2016 ◽  
pp. 1-11 ◽  
Author(s):  
M. A. Anacleto ◽  
D. Bazeia ◽  
F. A. Brito ◽  
J. C. Mota-Silva
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Specific Heat ◽  
Black Hole Entropy ◽  
Jacobi Method ◽  
Thermodynamic Quantities ◽  
Two Dimensional ◽  
Uncertainty Principles ◽  
Lifshitz Black Holes ◽  
Lifshitz Black Hole

We focus on the Hamilton-Jacobi method to determine several thermodynamic quantities such as temperature, entropy, and specific heat of two-dimensional Horava-Lifshitz black holes by using the generalized uncertainty principles (GUP). We also address the product of horizons, mainly concerning the event, Cauchy, and cosmological and virtual horizons.

CAN SMALL TWO-DIMENSIONAL BLACK HOLES EXIST?

1987 ◽  
Vol 02 (08) ◽  
pp. 555-560 ◽  
Author(s):  
O. J. KWON ◽  
B. H. CHO ◽  
Y. S. MYUNG
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Two Dimensional ◽  
Classical Stability ◽  
Dimensional Black Hole ◽  
Pure Gravity

We discuss the classical stability of a two-dimensional black hole which arises from the Jackiw model and pure gravity with a curvature squared term. For both these two models, we find that there exists the exponentially growing mode with time. Therefore, it seems that a two-dimensional black hole does not truly exist.

scholarly journals Embedding into flat spacetime and black hole thermodynamics

2019 ◽  
Vol 35 (05) ◽  
pp. 2050013 ◽  
Author(s):  
T. R. Govindarajan ◽  
Sumanta Chakraborty
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Thermodynamic Description ◽  
Scaling Law ◽  
Black Hole Entropy ◽  
Flat Spacetime ◽  
Higher Dimensional ◽  
Black Hole Spacetime ◽  
Symmetric Black Hole ◽  
Black Hole Temperature

It is known that static and spherically symmetric black hole solutions of general relativity in different spacetimes can be embedded into higher-dimensional flat spacetime. Given this result, we have explored the thermodynamic nature of black holes á la its embedding into flat spacetime. In particular, we have explicitly demonstrated that black hole temperature can indeed be determined starting from the embedding and hence mapping of the static observers in black hole spacetime to Rindler observers in flat spacetime. Furthermore, by considering the dynamics of a scalar field in the flat spacetime, it is indeed possible to arrive at the area scaling law for black hole entropy. Thus, by using the flat spacetime field theory, one can indeed provide a thermodynamic description of black holes. Implications are also discussed.

scholarly journals SYMMETRIES, HORIZONS AND BLACK HOLE ENTROPY

2008 ◽  
Vol 17 (03n04) ◽  
pp. 659-664 ◽  
Author(s):  
S. CARLIP
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Degrees Of Freedom ◽  
Conformal Symmetry ◽  
Goldstone Boson ◽  
Thermal Characteristics ◽  
Black Hole Entropy ◽  
Conformal Anomaly ◽  
Two Dimensional ◽  
Statistical Mechanical

Black holes behave as thermodynamic systems, and a central task of any quantum theory of gravity is to explain these thermal properties. A statistical-mechanical description of black hole entropy once seemed remote, but today we suffer an embarrassment of riches: despite counting very different states, many inequivalent approaches to quantum gravity obtain identical results. Such "universality" may reflect an underlying two-dimensional conformal symmetry near the horizon, which can be powerful enough to control the thermal characteristics independent of other details of the theory. This picture suggests an elegant description of the relevant degrees of freedom as Goldstone-boson-like excitations arising from symmetry breaking by the conformal anomaly.

Two dimensional black hole entropy

2007 ◽  
Vol 53 (1) ◽  
pp. 95-97 ◽  
Author(s):  
J. Sadeghi ◽  
M.R. Setare ◽  
B. Pourhassan
Keyword(s):  
Black Hole ◽  
Black Hole Entropy ◽  
Two Dimensional ◽  
Dimensional Black Hole

scholarly journals On thermodynamics of 2D black holes in brane inflationary potentials

2014 ◽  
Vol 11 (05) ◽  
pp. 1450047 ◽  
Author(s):  
A. Belhaj ◽  
M. Chabab ◽  
H. El Moumni ◽  
M. B. Sedra ◽  
A. Segui
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Black Hole Solution ◽  
Brane World ◽  
Two Dimensional ◽  
Dilaton Gravity ◽  
De Sitter ◽  
Asymptotic Behaviors ◽  
Dimensional Black Hole ◽  
Hole Geometry

Inspired from the inflation brane world cosmology, we study the thermodynamics of a black hole solution in two-dimensional dilaton gravity with an arctangent potential background. We first derive the two-dimensional black hole geometry, then we examine its asymptotic behaviors. More precisely, we find that such behaviors exhibit properties appearing in some known cases including the anti-de Sitter and the Schwarzschild black holes. Using the complex path method, we compute the Hawking radiation. The entropy function can be related to the value of the potential at the horizon.

scholarly journals Universality of highly damped quasinormal modes for single horizon black holes

2006 ◽  
Vol 84 (6-7) ◽  
pp. 473-479
Author(s):  
R G Daghigh ◽  
G Kunstatter
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Large Class ◽  
Quasinormal Modes ◽  
Black Hole Entropy ◽  
Mode Frequency ◽  
Quasinormal Mode ◽  
Asymptotically Flat ◽  
Black Hole Temperature

It has been suggested that the highly damped quasinormal modes of black holes provide information about the microscopic quantum gravitational states underlying black-hole entropy. This interpretation requires the form of the highly damped quasinormal mode frequency to be universally of the form: [Formula: see text] = ln(l)kTBH, where l is an integer, and TBH is the black-hole temperature. We summarize the results of an analysis of the highly damped quasinormal modes for a large class of static single horizon, asymptotically flat black holes.PACS Nos.: 04.60.–m, 04.70.–s, 04.70.Dy, 04.70.Bw, 92.60.Dj

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