共查询到20条相似文献,搜索用时 31 毫秒
1.
Jun Ren 《International Journal of Theoretical Physics》2009,48(2):431-440
The understanding of possible role played by the inner horizon of black holes in black hole thermodynamics is still somewhat
incomplete. By adopting Damour-Ruffini method and the thin film model which is developed on the base of brick wall model suggested
by ’t Hooft, we calculate the temperature and the entropy of the inner horizon of a R-N black hole. We conclude that the temperature
of inner horizon is positive and the entropy of the inner horizon is proportional to the area of the inner horizon. In addition,
the cut-off factor is 90β, which is same in calculation of the entropy of the outer horizon. So, we prove the existence of thermal characters of the
inner horizon. Then, we discuss that if the contribution of the inner horizon is taken into account to the total entropy of
the black hole, the Nernst theorem can be satisfied. At last, we study the tunneling effect including the inner horizon of
the Reissner-Nordstrom black hole. We calculate the tunneling rate of the outer horizon Γ+ and the inner horizon Γ−. The total tunneling rate Γ should be the product of the rates of the outer and inner horizon, Γ=Γ+⋅Γ−. We find that the total tunneling rate is in agreement with the Parikh’s standard result, Γ→exp (ΔS
BH
), and there is no information loss. 相似文献
2.
Jun Ren 《International Journal of Theoretical Physics》2009,48(7):2088-2097
In this paper, we study the thermal properties of the inner horizon of a Kerr-Newman black hole. By adopting Damour-Ruffini
method and the thin film model which is developed on the base of brick wall model suggested by ’t Hooft, we calculate the
temperature and the entropy of the inner horizon of a Kerr-Newman black hole. We conclude that the temperature of inner horizon
is positive and the entropy of the inner horizon is proportional to the area of the inner horizon. The cut-off factor is same
as it in calculation of the entropy of the outer horizon, 90β. In addition, we write the integral and differential Bekenstein-Smarr formula as the parameters of the inner horizon. Then,
we discuss that if the contribution of the inner horizon is taken into account to the total entropy of the black hole, the
Nernst theorem can be satisfied. At last, We calculate the tunneling rate of the outer horizon Γ+ and the inner horizon Γ−. The total tunneling rate Γ should be the product of the rates of the outer and inner horizon, Γ=Γ+⋅Γ−. We find that the total tunneling rate is in agreement with the Parikh’s standard result, Γ→exp (ΔS
BH
), and there is no information loss. 相似文献
3.
The horizon (the surface) of a black hole is a null surface, defined by those hypothetical “outgoing” light rays that just
hover under the influence of the strong gravity at the surface. Because the light rays are orthogonal to the spatial two-dimensional
surface at one instant of time, the surface area of the black hole is the same for all observers (i.e. the same for all coordinate
definitions of “instant of time”). This value is 4π(2Gm/c
2)2 for nonspinning black holes, with G = Newton’s constant, c = speed of light, and m = mass of the black hole. The three-dimensional spatial volume inside a black hole, in contrast, depends explicitly on the
definition of time, and can even be time dependent, or zero. We give examples of the volume found inside a standard, nonspinning
spherical black hole, for several different standard time-coordinate definitions. Elucidating these results for the volume
provides a new pedagogical resource of facts already known in principle to the relativity community, but rarely worked out. 相似文献
4.
We investigate quantum entanglement of gravitational configurations in 3D AdS gravity using the AdS/CFT correspondence. We
derive explicit formulas for the holographic entanglement entropy (EE) of the BTZ black hole, conical singularities and regularized
AdS3. The leading term in the large temperature expansion of the holographic EE of the BTZ black hole reproduces exactly its Bekenstein-Hawking
entropy S
BH
, whereas the subleading term behaves as ln S
BH
. We also show that the leading term of the holographic EE for the BTZ black hole can be obtained from the large temperature
expansion of the partition function of a broad class of 2D CFTs on the torus. This result indicates that black hole EE is
not a fundamental feature of the underlying theory of quantum gravity but emerges when the semiclassical notion of spacetime
geometry is used to describe the black hole. 相似文献
5.
Molin Liu Junwang Lu Yonglei Jia Jianbo Lu 《International Journal of Theoretical Physics》2011,50(6):1978-1989
In this paper we investigate quantum statistical entropy for the Kehagias-Sfetsos black hole in IR modified Hořava-Lifshitz
gravity by using t’ Hooft’s brick-wall method and generalized uncertainty principle method. By carefully calculating, we obtain
the brick-wall entropy S
BWM
=A/4 and the generalized uncertainty principle entropy S
GUP
=A/96πγ. It is found if we view from quantum statistics, the brick-wall entropy and generalized uncertainty principle entropy may
possibly is proportional to the event horizon area. This type area entropy is also justified by Wang et al. (Phys. Rev. D
81:083006, 2010). The study of the quantum statistical entropy may shed light on the understand of Hořava-Lifshitz gravity. 相似文献
6.
S. Carlip 《International Journal of Theoretical Physics》2007,46(9):2192-2203
Black hole entropy appears to be “universal”—many independent calculations, involving models with very different microscopic
degrees of freedom, all yield the same density of states. I discuss the proposal that this universality comes from the behavior
of the underlying symmetries of the classical theory. To impose the condition that a black hole be present, we must partially
break the classical symmetries of general relativity, and the resulting Goldstone-boson-like degrees of freedom may account
for the Bekenstein–Hawking entropy. In particular, I demonstrate that the imposition of a “stretched horizon” constraint modifies
the algebra of symmetries at the horizon, allowing the use of standard conformal field theory techniques to determine the
asymptotic density of states. The results reproduce the Bekenstein–Hawking entropy without any need for detailed assumptions
about the microscopic theory. 相似文献
7.
We find solution to the metric function f(r) = 0 of charged BTZ black hole making use of the Lambert function. The condition of extremal charged BTZ black hole is determined
by a non-linear relation of M
e
(Q) = Q
2(1 − ln Q
2). Then, we study the entropy of extremal charged BTZ black hole using the entropy function approach. It is shown that this
formalism works with a proper normalization of charge Q for charged BTZ black hole because AdS2 × S1 represents near-horizon geometry of the extremal charged BTZ black hole. Finally, we introduce the Wald’s Noether formalism
to reproduce the entropy of the extremal charged BTZ black hole without normalization when using the dilaton gravity approach. 相似文献
8.
Mario Rabinowitz 《International Journal of Theoretical Physics》2006,45(5):851-858
The simplest possible equation for Hawking radiation and other black hole radiated power is derived in terms of black hole density, ρ . Black hole density also leads to the simplest possible model of a gas of elementary constituents confined inside a gravitational bottle of Schwarzchild radius at tremendous pressure, which yields identically the same functional dependence as the traditional black hole entropy S
bh∝ (kAc
3)/ℏ G. Variations of S
bh can be obtained which depend on the occupancy of phase space cells. A relation is derived between the constituent momenta and the black hole radius R
H, p = which is similar tothe Compton wavelength relation. 相似文献
9.
Dumitru Astefanesei Kevin Goldstein Swapna Mahapatra 《General Relativity and Gravitation》2008,40(10):2069-2105
We investigate four-dimensional spherically symmetric black hole solutions in gravity theories with massless, neutral scalars
non-minimally coupled to gauge fields. In the non-extremal case, we explicitly show that, under the variation of the moduli,
the scalar charges appear in the first law of black hole thermodynamics. In the extremal limit, the near horizon geometry
is AdS
2 × S
2 and the entropy does not depend on the values of moduli at infinity. We discuss the attractor behaviour by using Sen’s entropy
function formalism as well as the effective potential approach and their relation with the results previously obtained through
special geometry method. We also argue that the attractor mechanism is at the basis of the matching between the microscopic
and macroscopic entropies for the extremal non-BPS Kaluza–Klein black hole. 相似文献
10.
Considering the back-reaction of emitting particles to the black hole, a “new” horizon is suggested where thermodynamics can
be built in the dynamical black hole. It, at least, means that the thermodynamics of a dynamical black hole should not be
constructed at the original event horizon any more. The temperature, “new” horizon position and radiating particles’ energy
will be consistent again under the theory of equilibrium thermodynamical system.
相似文献
11.
G. A. Kozlov 《Physics of Particles and Nuclei》2010,41(6):954-956
A field model for a quark and an antiquark binding is described. Quarks interact via a gauge unparticle (“ungluon”). The model
is formulated in terms of Lagrangian which features the source field S(x) which becomes a local pseudo-Goldstone field of conformal symmetry — the pseudodilaton mode and from which the gauge non-primary
unparticle field is derived by B
μ(x) ∼ ∂μ
S(x). Because the conformal sector is strongly coupled, the mode S(x) may be one of new states accessible at high energies. We have carried out an analysis of the important quantity that enters
in the “ungluon” exchange pattern — the “ungluon” propagator. 相似文献
12.
Daniel Wilkins 《General Relativity and Gravitation》1979,11(1):45-58
Bekenstein and Hawking saved the second law of thermodynamics near a black hole by assigning to the hole an entropyS h proportional to the area of its event horizon. It is tempting to assume thatS h possesses all the features commonly associated with the physical entropy. Kundt has shown, however, thatS h violates several reasonable physical expectations. We review his criticism, augmenting it as follows: (a)S h is a badly behaved state function requiring knowledge of the hole's future history; and (b) close analogs of event horizons in other space-times do not possess an “entropy.” We also discuss these questions: (c) IsS h suitable for all regions of a black-hole space-time? And (b) shouldS h be attributed to the exterior of a white hole? One can retainS h for the interior (respectively, exterior) of a black (respectively, white) hole, but we reject this as contrary to the information-theoretic derivation of horizon entropy given by Bekenstein. The total entropy defined by Kundt (all ordinary entropy on space-section cutting through the hole, no horizon term) and that of Bekenstein-Hawking (ordinary entropy outside horizon plus horizon term) appear to be complementary concepts with separate domains of validity. In the most natural choice, an observer inside a black hole will use Kundt's entropy, and one remaining outside that of Bekenstein-Hawking. 相似文献
13.
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
14.
M. B. Mensky 《Optics and Spectroscopy》2007,103(3):461-467
Conceptual problems in quantum mechanics result from the specific quantum concept of reality and require, for their solution,
including the observer’s consciousness into the quantum theory of measurements. Most naturally, this is achieved in the framework
of Everett’s “many-world interpretation” of quantum mechanics. According to this interpretation, various classical alternatives
are perceived by consciousness separately from each other. In the Extended Everett Concept (EEC) proposed by the present author,
the separation of the alternatives is identified with the phenomenon of consciousness. This explains the classical character of the alternatives and unusual manifestations
of consciousness arising “at the edge of consciousness” (i.e., in sleep or trance) when its access to “other alternative classical
realities” (other Everett’s worlds) becomes feasible. Because of reversibility of quantum evolution in EEC, all time moments
in the quantum world are equivalent, while the impression of flow of time appears only in consciousness. If it is assumed
that consciousness may influence the probabilities of alternatives (which is consistent in case of infinitely many Everett’s
worlds), EEC explains free will, “probabilistic miracles” (observing low-probability events), and decreasing entropy in the
sphere of life.
The text was submitted by the author in English. 相似文献
15.
J. R. Mureika 《International Journal of Theoretical Physics》2012,51(4):1259-1267
Vector unparticle couplings to standard model fields produce repulsive corrections to gravity. From a general relativistic
perspective, this leads to an effective Reissner-Nordstr?m-like metric whose “charge” is a function of the unparticle coupling
constant λ, and therefore can admit naked singularities. Requiring the system to respect cosmic censorship provides a new method of
constraining the value of λ. These limits are extremely loose for stellar-mass black holes, but commensurate with existing bounds for primordial black
holes. In the case of theoretical low-mass black holes, the bounds on λ are much stricter than those derived from astrophysical and accelerator phenomenology. Additional constraints on the lower
limit of λ are used to estimate the mass of the smallest possible black hole MBHminM_{\mathrm {BH}}^{\mathrm{min}} that can be formed in the unparticle framework, as a function of the unparticle parameters (LU,MU,dU,dBZ\Lambda_{{\mathcal{U}}},M_{{\mathcal{U}}},{d_{\mathcal{U}}},{d_{\mathit{BZ}}}). 相似文献
16.
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
17.
A. E. Shalyt-Margolin 《Optics and Spectroscopy》2007,103(2):264-266
It is noted that in the quantum theory at Planck’s scales (Early Universe), with introduction of the fundamental length, the
measuring procedure is changed, leading to the density-matrix deformation. This deformation is described explicitly, and its
inferences may be used for the determination of pure and mixed states in the associated quantum mechanics, for Hawking’s Problem
solution in case of the coherence loss on black hole evaporation, and in calculations of the black hole quantum entropy.
The text was submitted by the author in English. 相似文献
18.
An event horizon for “relativistic” fermionic quasiparticles can be constructed in a thin film of superfluid 3He-A. The quasiparticles see an effective “gravitational” field which is induced by a topological soliton of the order parameter.
Within the soliton the “speed of light” crosses zero and changes sign. When the soliton moves, two planar event horizons (black
hole and white hole) appear, with a curvature singularity between them. Aside from the singularity, the effective spacetime
is incomplete at future and past boundaries, but the quasiparticles cannot escape there because the nonrelativistic corrections
become important as the blueshift grows, yielding “superluminal” trajectories. The question of Hawking radiation from the
moving soliton is discussed but not resolved.
Pis’ma Zh. éksp. Teor. Fiz. 68, No. 11, 833–838 (10 December 1998)
Published in English in the original Russian journal. Edited by Steve Torstveit. 相似文献
19.
Thomas A. Roman 《General Relativity and Gravitation》1988,20(4):359-370
We consider the rate at which energy can be extracted from a charged black hole using the mining process developed by Unruh and Wald. It is shown that for a Reissner-Nordström black hole the mining rate depends on the mass of the hole (unlike in the Schwarzschild case) and goes to zero asT
BH 0. We also argue that it is impossible to achieveT
BH=0 in a finite time by mining. 相似文献
20.
Steven Weinstein 《Foundations of Physics》2009,39(8):921-936
Bell’s theorem is purported to demonstrate the impossibility of a local “hidden variable” theory underpinning quantum mechanics.
It relies on the well-known assumption of ‘locality’, and also on a little-examined assumption called ‘statistical independence’
(SI). Violations of this assumption have variously been thought to suggest “backward causation”, a “conspiracy” on the part of
nature, or the denial of “free will”. It will be shown here that these are spurious worries, and that denial of SI simply implies nonlocal correlation between spacelike degrees of freedom. Lorentz-invariant theories in which SI does not hold are easily constructed: two are exhibited here. It is conjectured, on this basis, that quantum-mechanical phenomena
may be modeled by a local theory after all.
This paper is dedicated to the memory of John A. Wheeler. 相似文献