scholarly journals The Phase Transition of Higher Dimensional Charged Black Holes

2016 ◽  
Vol 2016 ◽  
pp. 1-10 ◽  
Author(s):  
Xiongying Guo ◽  
Huaifan Li ◽  
Lichun Zhang ◽  
Ren Zhao
Keyword(s):  
Black Hole ◽  
Critical Point ◽  
Intrinsic Property ◽  
Flat Space ◽  
Thermodynamic System ◽  
Asymptotically Flat ◽  
Black Hole Thermodynamic ◽  
Charged Black Holes ◽  
Higher Dimensional ◽  
Ads Spacetime

We have studied phase transitions of higher dimensional charge black hole with spherical symmetry. We calculated the local energy and local temperature and find that these state parameters satisfy the first law of thermodynamics. We analyze the critical behavior of black hole thermodynamic system by taking state parameters(Q,Φ)of black hole thermodynamic system, in accordance with considering the state parameters(P,V)of van der Waals system, respectively. We obtain the critical point of black hole thermodynamic system and find that the critical point is independent of the dual independent variables we selected. This result for asymptotically flat space is consistent with that for AdS spacetime and is intrinsic property of black hole thermodynamic system.

scholarly journals Islands and stretched horizon

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Yoshinori Matsuo
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Radiation ◽  
Entanglement Entropy ◽  
Total System ◽  
Island Rule ◽  
Asymptotically Flat ◽  
Flat Spacetime ◽  
Ads Spacetime ◽  
Hole Geometry

Abstract Recently it was proposed that the entanglement entropy of the Hawking radiation contains the information of a region including the interior of the event horizon, which is called “island.” In studies of the entanglement entropy of the Hawking radiation, the total system in the black hole geometry is separated into the Hawking radiation and black hole. In this paper, we study the entanglement entropy of the black hole in the asymptotically flat Schwarzschild spacetime. Consistency with the island rule for the Hawking radiation implies that the information of the black hole is located in a different region than the island. We found an instability of the island in the calculation of the entanglement entropy of the region outside a surface near the horizon. This implies that the region contains all the information of the total system and the information of the black hole is localized on the surface. Thus the surface would be interpreted as the stretched horizon. This structure also resembles black holes in the AdS spacetime with an auxiliary flat spacetime, where the information of the black hole is localized at the interface between the AdS spacetime and the flat spacetime.

scholarly journals The Thermodynamic Relationship between the RN-AdS Black Holes and the RN Black Hole in Canonical Ensemble

2017 ◽  
Vol 2017 ◽  
pp. 1-7 ◽  
Author(s):  
Yu-Bo Ma ◽  
Li-Chun Zhang ◽  
Jian Liu ◽  
Ren Zhao ◽  
Shuo Cao
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Flat Space ◽  
Space Time ◽  
Asymptotically Flat ◽  
Time Space ◽  
Ads Black Holes ◽  
Different Types ◽  
Thermodynamic Relationship ◽  
The Relationship

In this paper, by analyzing the thermodynamic properties of charged AdS black hole and asymptotically flat space-time charged black hole in the vicinity of the critical point, we establish the correspondence between the thermodynamic parameters of asymptotically flat space-time and nonasymptotically flat space-time, based on the equality of black hole horizon area in the two different types of space-time. The relationship between the cavity radius (which is introduced in the study of asymptotically flat space-time charged black holes) and the cosmological constant (which is introduced in the study of nonasymptotically flat space-time) is determined. The establishment of the correspondence between the thermodynamics parameters in two different types of space-time is beneficial to the mutual promotion of different time-space black hole research, which is helpful to understand the thermodynamics and quantum properties of black hole in space-time.

scholarly journals THE CARDY–VERLINDE FORMULA AND ASYMPTOTICALLY FLAT CHARGED BLACK HOLES

2001 ◽  
Vol 16 (19) ◽  
pp. 1263-1268 ◽  
Author(s):  
DONAM YOUM
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Casimir Effect ◽  
Higher Dimensions ◽  
Thermodynamic Quantities ◽  
Two Dimensional ◽  
Temperature Relation ◽  
Asymptotically Flat ◽  
Charged Black Holes ◽  
Verlinde Formula

We show that the modified Cardy–Verlinde formula without the Casimir effect term is satisfied by asymptotically flat charged black holes in arbitrary dimensions. Thermodynamic quantities of the charged black holes are shown to satisfy the energy-temperature relation of a two-dimensional CFT, which supports the claim in our previous work (Phys. Rev.D61, 044013, hep-th/9910244) that thermodynamics of charged black holes in higher dimensions can be effectively described by two-dimensional theories. We also check the Cardy formula for the two-dimensional black hole compactified from a dilatonic charged black hole in higher dimensions.

scholarly journals SPECTROSCOPY OF AN AdS REISSNER–NORDSTRØM BLACK HOLE

2006 ◽  
Vol 15 (03) ◽  
pp. 439-457 ◽  
Author(s):  
CLAUDIO DAPPIAGGI ◽  
SIMONA RASCHI
Keyword(s):  
Black Hole ◽  
Cosmological Constant ◽  
Flat Space ◽  
Space Time ◽  
Charged Black Hole ◽  
Area Spectrum ◽  
Asymptotically Flat ◽  
Negative Cosmological Constant

In the framework of black hole spectroscopy, we extend the results obtained for a charged black hole in an asymptotically flat space–time to the scenario with non-vanishing negative cosmological constant. In particular, exploiting Hamiltonian techniques, we construct the area spectrum for an AdS Reissner–Nordstrøm black hole.

QUANTUM DISCORD AND QUANTUM ENTANGLEMENT IN THE PRESENCE OF AN ASYMPTOTICALLY FLAT STATIC BLACK HOLE

2013 ◽  
Vol 11 (06) ◽  
pp. 1350061
Author(s):  
EYLEE JUNG ◽  
MI-RA HWANG ◽  
DAEKIL PARK
Keyword(s):  
Black Hole ◽  
Quantum Discord ◽  
Full Range ◽  
Flat Space ◽  
Hawking Temperature ◽  
Classical Correlation ◽  
Asymptotically Flat ◽  
W States ◽  
Static Black Hole ◽  
Space Limit

In this work, the quantum discord and tripartite entanglement in the presence of an asymptotically flat static black hole are discussed. The total correlation, quantum discord, and classical correlation are found to exhibit decreasing behavior with increasing Hawking temperature. It is shown that the classical correlation is less than the quantum discord in the full range of Hawking temperature. The tripartite entanglements for Greenberger–Horne–Zeilinger (GHZ) and W-states also exhibit decreasing behavior with increasing Hawking temperature. When the Hawking temperature approaches the infinite limit, the tripartite entanglements of the GHZ and W-states reduce, in terms of the π-tangle, to 52% and 33% of the corresponding values in the flat space limit, respectively.

scholarly journals BRANE WORLD IN A TOPOLOGICAL BLACK HOLES IN ASYMPTOTICALLY FLAT SPACE–TIME

2001 ◽  
Vol 16 (26) ◽  
pp. 1703-1710 ◽  
Author(s):  
DONAM YOUM
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Flat Space ◽  
Space Time ◽  
Brane World ◽  
Black Hole Horizon ◽  
World Model ◽  
Asymptotically Flat ◽  
Bulk Scalar Field

We study static brane configurations in the bulk background of the topological black holes in asymptotically flat space–time and find that such configurations are possible even for flat black hole horizon, unlike the AdS black hole case. We construct the brane world model with an orbifold structure S1/Z2 in such bulk background and study massless bulk scalar field.

scholarly journals The Abrikosov vortex in curved space

2021 ◽  
Vol 2021 (9) ◽  
Author(s):  
Jan Albert
Keyword(s):  
Black Hole ◽  
The Self ◽  
Singular Solutions ◽  
Abrikosov Vortex ◽  
Btz Black Hole ◽  
Holographic Superconductor ◽  
Curved Space ◽  
Asymptotically Flat ◽  
Higher Dimensional ◽  
Vortex Solutions

Abstract We study the self-gravitating Abrikosov vortex in curved space with and with-out a (negative) cosmological constant, considering both singular and non-singular solutions with an eye to hairy black holes. In the asymptotically flat case, we find that non-singular vortices round off the singularity of the point particle’s metric in 3 dimensions, whereas singular solutions consist of vortices holding a conical singularity at their core. There are no black hole vortex solutions. In the asymptotically AdS case, in addition to these solutions there exist singular solutions containing a BTZ black hole, but they are always hairless. So we find that in contrast with 4-dimensional ’t Hooft-Polyakov monopoles, which can be regarded as their higher-dimensional analogues, Abrikosov vortices cannot hold a black hole at their core. We also describe the implications of these results in the context of AdS/CFT and propose an interpretation for their CFT dual along the lines of the holographic superconductor.

scholarly journals Extremal black holes that are not extremal: maximal warm holes

2022 ◽  
Vol 2022 (1) ◽  
Author(s):  
Óscar J. C. Dias ◽  
Gary T. Horowitz ◽  
Jorge E. Santos
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Hawking Temperature ◽  
Charged Scalar ◽  
Asymptotically Flat ◽  
Charged Black Holes ◽  
Maximum Charge ◽  
Scalar Hair ◽  
Hairy Black Hole ◽  
Extremal Black Holes

Abstract We study a family of four-dimensional, asymptotically flat, charged black holes that develop (charged) scalar hair as one increases their charge at fixed mass. Surprisingly, the maximum charge for given mass is a nonsingular hairy black hole with nonzero Hawking temperature. The implications for Hawking evaporation are discussed.

scholarly journals NONPERTURBATIVE INSTABILITY OF BLACK HOLES IN QUANTUM GRAVITY

1989 ◽  
Vol 04 (16) ◽  
pp. 1497-1507 ◽  
Author(s):  
PAWEL O. MAZUR
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Quantum Gravity ◽  
Unstable Mode ◽  
General Setting ◽  
Flat Space ◽  
Hawking Effect ◽  
Decay Channels ◽  
Asymptotically Flat ◽  
Minimal Sphere

The final stage of a black hole evaporation due to the Hawking effect is studied. One finds that, including the effects of quantum gravity, a black hole does not evaporate completely losing its energy steadily to a flux of created particles, but rather decays via a change in topology into an asymptotically flat space and an object which is a closed Friedmann Universe. This process is a genuine non-perturbative effect of quantum gravity and becomes the dominant “channel” of a black hole decay for black holes with masses slightly larger than the Planck mass Mp=1019 GeV. We calculate the decay rate of a Schwarzchild black hole with the mass M and discuss other decay “channels” by topology change. An explicit instanton mediating the decay is constructed by matching the Schwarzschild and the “wormhole” Friedmann instantons on the minimal sphere which is a Euclidean section of the event horizon. We show, as an example, that the decay process is mediated in the semi-classical approximation by the gravitational-axionic instanton. However, we argue that the phenomenon discussed in this paper does not depend on the particular instanton approximation and should be discussed in the framwork of the second quantization of interacting geometry suggested in Ref. 17. It is argued that in the more general setting of the Wheeler-De Witt equation, the wave functional describing a black hole is not gaussian because of the existence of an unstable mode.

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.

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