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1.
Donald Marolf 《General Relativity and Gravitation》2009,41(4):903-917
This brief conference proceeding attempts to explain the implications of the anti-de Sitter/conformal field theory (AdS/CFT)
correspondence for black hole entropy in a language accessible to relativists and other non-string theorists. The main conclusion
is that the Bekenstein–Hawking entropy S
BH
is the density of states associated with certain superselections sectors, defined by what may be called the algebra of boundary
observables. Interestingly while there is a valid context in which this result can be restated as “S
BH
counts all states inside the black hole,” there may also be another in which it may be restated as “S
BH
does not count all states inside the black hole, but only those that are distinguishable from the outside.” The arguments
and conclusions represent the author’s translation of the community’s collective wisdom, combined with a few recent results. 相似文献
2.
We find the existence of a quantum thermal effect, “Hawking absorption.” near the inner horizon of the Kerr–Newman black hole. Redefining the entropy, temperature, angular velocity, and electric potential of the black hole, we give a new formulation of the Bekenstein–Smarr formula. The redefined entropy vanishes for absolute zero temperature of the black hole and hence it is interpreted as the Planck absolute entropy of the KN black hole. 相似文献
3.
It has often been suggested (especially by S. Carlip) that spacetime symmetries in the neighborhood of a black hole horizon
may be relevant to a statistical understanding of the Bekenstein–Hawking entropy. A prime candidate for this type of symmetry
is that one which is exhibited by the Einstein tensor. More precisely, it is now known that this tensor takes on a strongly
constrained (block-diagonal) form as it approaches any stationary, non-extremal Killing horizon. Presently, exploiting the
geometrical properties of such horizons, we provide a particularly elegant argument that substantiates this highly symmetric
form for the Einstein tensor. It is, however, duly noted that, on account of a “loophole,” the argument does fall just short
of attaining the status of a rigorous proof. 相似文献
4.
The Bekenstein–Hawking entropy of certain black holes can be computed microscopically in string theory by mapping the elusive
problem of counting microstates of a strongly gravitating black hole to the tractable problem of counting microstates of a
weakly coupled D-brane system, which has no event horizon, and indeed comfortably fits on the head of a pin. We show here
that, contrary to widely held beliefs, the entropy of spherically symmetric black holes can easily be dwarfed by that of stationary
multi-black-hole “molecules” of the same total charge and energy. Thus, the corresponding pin-sized D-brane systems do not
even approximately count the microstates of a single black hole, but rather those of a zoo of entropically dominant multicentered
configurations.
Fourth Award in the 2007 Essay Competition of the Gravity Research Foundation. 相似文献
5.
Considering the unfixed background space-time and self-gravitational interaction, we review the Hawking radiation of the Kerr–Newman
black hole by Hamilton–Jacobi method. The result shows the tunneling probability is related to the change of Bekenstein–Hawking
entropy and the radiation spectrum deviates from the precisely thermal one, which is in accordance with Parikh and Wilczek’s
result and gives another method to study the Hawking radiation of the black hole. 相似文献
6.
Qing-Quan Jiang Wei Ren Jian Tang Xiao-Feng Liu 《International Journal of Theoretical Physics》2007,46(6):1449-1454
Applying the semi-classical quantum tunneling model, we have studied the Hawking radiation via tunneling from a cylindrically
symmetric black hole. The derived results show that the tunneling rate of at the event horizon of the black hole is related
to Bekenstein–Hawking entropy and the factual radiation spectrum is not strictly pure thermal, but is consistent with the
underlying unitary theory.
PACS numbers: 04.20.-s, 97.60.Lf. 相似文献
7.
We investigate the thermodynamic properties of 5D static and spherically symmetric black holes in (i) Einstein–Maxwell–Gauss–Bonnet
theory, (ii) Einstein–Maxwell–Gauss–Bonnet theory with negative cosmological constant, and in (iii) Einstein–Yang–Mills–Gauss–Bonnet
theory. To formulate the thermodynamics of these black holes we use the Bekenstein–Hawking entropy relation and, alternatively,
a modified entropy formula which follows from the first law of thermodynamics of black holes. The results of both approaches
are not equivalent. Using the formalism of geometrothermodynamics, we introduce in the manifold of equilibrium states a Legendre
invariant metric for each black hole and for each thermodynamic approach, and show that the thermodynamic curvature diverges
at those points where the temperature vanishes and the heat capacity diverges. 相似文献
8.
Applying the Hamilton–Jacobi method, we investigate the Hawking radiation as tunneling from the non-stationary Vaidya–Bonner
black hole by considering the unfixed background space-time and self-gravitational interaction. The result shows the actual
radiation spectrum deviates from the purely thermal one and the tunneling rate is related not only to the change of Bekenstein–Hawking
entropy but also to the integral to the black hole mass and charge. This implies information loss is possible. 相似文献
9.
There is much attention on the corrections to Bekenstein–Hawking entropy in area with a model-dependent coefficient. The corrections
are generally composed of two parts: quantum corrections and thermal corrections. The generalized uncertainty principle (GUP),
which will reduce to the conventional Heisenberg relation in situations of weak gravity, is one of the candidates to be utilized
to obtain the quantum corrections to the Bekenstein–Hawking entropy. Recently the extended uncertainty principle (EUP) and
generalized extended uncertainty principle (GEUP) are introduced to calculate entropy corrections with large length scales
limit. In this paper, we obtain the quantum corrections to Bekenstein–Hawking entropy in four-dimensional Schwarzschild black
holes based on the EUP and GEUP. Some attractive results are derived. 相似文献
10.
Juan Yang 《International Journal of Theoretical Physics》2009,48(9):2592-2598
Via the method beyond semi-classical approximation, we obtain the correctional tunneling probability and Hawking temperature
at the apparent horizon of Finsler rainbow universe. Then we apply Bekenstein–Hawking entropy area law used in black hole
to the cases of rainbow universe, and reach the entropy of the apparent horizon. Finally, we calculate the correctional entropy
and obtain reasonable results. 相似文献
11.
It is shown that non-rotating black holes in three or four dimensions possess a canonical entropy. Recently study indicated
that there were logarithmic corrections to Bekenstein–Hawking entropy in area with a uncertain coefficient which depends on
specific models. In this paper, the thermal fluctuations on Bekenstein–Hawking entropy in five-dimensional topological AdS
(TAds)-black holes and topological de Sitter (Tds) spaces will be considered based on a uniformly spaced area spectrum approach. 相似文献
12.
Yun Soo Myung Myungseok Yoon 《The European Physical Journal C - Particles and Fields》2009,62(2):405-411
We find a new black hole in three-dimensional anti-de Sitter space by introducing an anisotropic perfect fluid inspired by
the noncommutative black hole. This is a regular black hole with two horizons. We compare the thermodynamics of this black
hole with that of a non-rotating BTZ black hole. The first-law of thermodynamics is not compatible with the Bekenstein–Hawking
entropy. 相似文献
13.
Kerner and Mann’s recent research shows that the Hawking temperature and tunneling rate can be obtained by the fermion tunneling
method from the Rindler space-time and a general non-rotating black hole. In this paper, considering the tunneling particles
with spin 1/2 and taking into account the particle’s self-gravitation in the dynamical background space-time, we further improve
Kerner and Man’s fermion tunneling method to investigate Hawking radiation via tunneling from a non-static black hole with
the internal global monopole. The result shows that the tunneling rate of the non-static black hole is related to the integral
of the changing horizon besides the change of Bekenstein–Hawking entropy, which is different from the stationary cases. It
also essentially implies that the unitary is violated for the reason that the black hole is non-stationary and cannot be treated
as an isolated system. 相似文献
14.
S. Carlip 《General Relativity and Gravitation》2007,39(10):1519-1523
15.
ShuZheng Yang HuiLing Li QingQuan Jiang 《International Journal of Theoretical Physics》2006,45(5):965-972
Taking energy conservation and angular momentum conservation into account, the tunneling radiation characteristics of stationary axisymmetric Sen black hole is studied in this paper with the quantum tunneling method and the results show that the tunneling rate of particle at the event horizon of the black hole is relevant to Bekenstein–Hawking entropy and that the radiation spectrum is not strictly pure thermal.
PACS: 04.70_S, 97.60.Lf 相似文献
16.
Black Hole Entropy: Membrane Approach 总被引:1,自引:0,他引:1
The wall contribution character of the Bekenstein–Hawking entropy in the brick-wall model leads us to propose a new method of computing the entropy of a black hole. In our model, the entropy is attributed to the dynamical degrees of the field covering the two dimensional membranes just outside the horizon. A cutoff different from the model of 't Hooft is necessarily introduced. It can be treated as an increase in horizon because of the space–time fluctuations. It is also shown that our method can be applied to the nonstatic case, such as Vaidya–deSitter space–time, and the final result relies on a time-dependent cutoff different from the brick-wall model. 相似文献
17.
We extend the recently proposed Kerr/CFT correspondence to examine the dual conformal field theory of four-dimensional Kaluza–Klein black hole in Einstein–Maxwell–Dilaton theory. For the extremal Kaluza–Klein black hole, the central charge and temperature of the dual conformal field are calculated following the approach of Guica, Hartman, Song and Strominger. Meanwhile, we show that the microscopic entropy given by the Cardy formula agrees with Bekenstein–Hawking entropy of extremal Kaluza–Klein black hole. For the non-extremal case, by studying the near-region wave equation of a neutral massless scalar field, we investigate the hidden conformal symmetry of Kaluza–Klein black hole, and find the left and right temperatures of the dual conformal field theory. Furthermore, we find that the entropy of non-extremal Kaluza–Klein black hole is reproduced by Cardy formula. 相似文献
18.
Yu-Quan Yuan Xiao-Xiong Zeng Zhi-Jian Zhou Liang-Ping Jin 《General Relativity and Gravitation》2009,41(12):2771-2780
Recently, fermions tunneling beyond semiclassical approximation from an uncharged static black hole was investigated by Majhi,
which was based on the work of Banerjee and Majhi, it was found that the black hole entropy correction can be produced as
the quantum effect of a particle is taken into account. In this paper, we further extend this idea to the stationary Kerr
black hole to discuss its entropy correction. To get the corrections correctly, the proportionality parameters of quantum
corrections of action I
i
to the semiclassical action I
0 in this case are regarded as the inverse of the product of Planck Length and Planck Mass. The result shows that entropy corrections
to the stationary black hole also include the logarithmic term and inverse area term in Bekenstein–Hawking entropy beyond
semiclassical approximation. 相似文献
19.
20.
George Tsoupros 《General Relativity and Gravitation》2012,44(2):309-351
The analytic expression obtained in the preceding project for the massless conformal scalar propagator in the Hartle–Hawking
vacuum state for small values of the Schwarzschild radial coordinate above r = 2M is analytically extended into the interior of the Schwarzschild black hole. The result of the analytical extension coincides
with the exact propagator for a small range of values of the Schwarzschild radial coordinate below r = 2M and is an analytic expression which manifestly features its dependence on the background space–time geometry. This feature
as well as the absence of any assumptions and prerequisites in the derivation render this Hartle–Hawking scalar propagator
in the interior of the Schwarzschild black-hole geometry distinct from previous results. The two propagators obtained in the
interior and in the exterior region of the Schwarzschild black hole are matched across the event horizon. The result of that
match is a massless conformal scalar propagator in the Hartle–Hawking vacuum state which is shown to describe particle production
by the Schwarzschild black hole.
“The future is not what it used to be!” From Alan Parker’s film “Angel Heart” 相似文献