共查询到20条相似文献,搜索用时 296 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.
Bouetou Bouetou Thomas Mahamat Saleh Timoleon Crepin Kofane 《General Relativity and Gravitation》2012,44(9):2181-2189
We investigate thermodynamics and phase transition of the Reissner–Nordstr?m black hole surrounded by quintessence. Using thermodynamical laws of black holes, we derive the expressions of some thermodynamics quantities for the Reissner–Nordstr?m black hole surrounded by quintessence. The variations of the temperature and heat capacity with the entropy were plotted for different values of the state parameter related to the quintessence, ω q , and the normalization constant related to the density of quintessence c. We show that when varying the entropy of the black hole a phase transition is observed in the black hole. Moreover, when increasing the density of quintessence, the transition point is shifted to lower entropy and the temperature of the black hole decreases. 相似文献
4.
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
5.
利用黑洞热力学第一定律和第三定律分别导出黑洞的普朗克绝对熵公式,该公式表明黑洞熵与黑洞视界的全面积成正比.并进一步证明了黑洞的普朗克绝对熵就是经典热力学熵
关键词:
黑洞
视界
视界温度
普朗克绝对熵 相似文献
6.
Yun Soo Myung Yong-Wan Kim Young-Jai Park 《The European Physical Journal C - Particles and Fields》2008,58(2):337-346
We investigate the Gauss–Bonnet black hole in five dimensional anti-de Sitter spacetimes (GBAdS). We analyze all thermodynamic
quantities of the GBAdS, which is characterized by the Gauss–Bonnet coupling c and mass M, comparing with those of the Born–Infeld-AdS (BIAdS), Reissner–Norstr?m-AdS black holes (RNAdS), Schwarzschild-AdS (SAdS),
and BTZ black holes. For c<0 we cannot obtain the black hole with positively definite thermodynamic quantities of mass, temperature, and entropy, because
the entropy does not satisfy the area law. On the other hand, for c>0, we find the BIAdS-like black hole, showing that the coupling c plays the role of a pseudo-charge. Importantly, we could not obtain the SAdS in the limit of c→0, which means that the GBAdS is basically different from the SAdS. In addition, we clarify the connections between thermodynamic
and dynamical stability. Finally, we also conjecture that if a black hole is big and thus globally stable, its quasi-normal
modes may take on analytic expressions. 相似文献
7.
The entropy spectrum of a spherically symmetric black hole was derived via the Bohr–Sommerfeld quantization rule in Majhi and Vagenas’s work. Extending this work to charged and rotating black holes, we quantize the horizon area and the entropy of an Einstein–Maxwell–Dilaton–Axion black hole via the Bohr–Sommerfeld quantization rule and the adiabatic invariance. The result shows the area spectrum and the entropy spectrum are respectively equally spaced and independent on the parameters of the black hole. 相似文献
8.
Treating macro-black hole as quantum states, and using Brown–York's quasi-local gravitational energy definition and Heisenberg uncertainty principle, the GHS black hole's quantum horizon is constructed. The Hawking temperature is computed naturally, and the entropy can also be figured out without introducing the cutoff factor h. The Φ-field mode number is predicted too. The result is consistent with that of the Schwarzschild and R-N black hole. 相似文献
9.
Kenji Muneyuki Nobuyoshi Ohta 《The European Physical Journal C - Particles and Fields》2012,72(1):1858
We study Hawking radiation in a new class of black hole solutions in Einstein–Gauss–Bonnet theory. The black hole has been
argued to have vanishing mass and entropy, but finite Hawking temperature. To check if it really emits radiation, we analyze
Hawking radiation using the original method of quantization of a scalar field in the black hole background and with the quantum
tunneling method, and confirm that it emits radiation at the Hawking temperature. A general formula is derived for the Hawking
temperature and backreaction in the tunneling approach. Physical implications of these results are discussed. 相似文献
10.
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
11.
12.
Qing-Miao Meng Ji-Jian Jiang Jing-Lun Liu Zhong-Rang Li 《International Journal of Theoretical Physics》2010,49(8):1739-1745
Applying the entropy density near the event horizon, we obtained the result that the radiation energy flux of the black hole
is always proportional to the quartic of the temperature of its event horizon. That is to say, the thermal radiation of the
black hole always satisfies the generalized Stefan–Boltzmann law. The derived generalized Stefan–Boltzmann coefficient is
no longer a constant. When the cut-off distance and the thin film thickness are both fixed, it is a proportional coefficient
which is related to the black hole mass, the kinds of radiation particles and space–time metric near the event horizon. In
this paper, we have put forward a thermal particle model in curved space–time. By this model, the result has been obtained
that when the thin film thickness and the cut-off distance are both fixed, the radiation energy flux received by observer
far away from the Schwarzschild black hole is proportional to the average radial effusion velocity of the radiation particles
in the thin film, and inversely proportional to the square of the distance between the observer and the black hole. 相似文献
13.
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
14.
Recently, a Hamilton–Jacobi method beyond the semiclassical approximation in black hole physics was developed by Banerjee
and Majhi. We generalize their analysis of black holes to the case of a Friedmann–Robertson–Walker (FRW) universe. It is shown
that all the higher order quantum corrections in the single particle action are proportional to the usual semiclassical contribution.
The corrections to the Hawking-like temperature and entropy of the apparent horizon for the FRW universe are also obtained.
In the corrected entropy, the area law involves a logarithmic area correction together with the standard term with the inverse
power of the area. 相似文献
15.
Ashoke Sen 《General Relativity and Gravitation》2012,44(5):1207-1266
Logarithmic corrections to the extremal black hole entropy can be computed purely in terms of the low energy data—the spectrum
of massless fields and their interaction. The demand of reproducing these corrections provides a strong constraint on any
microscopic theory of quantum gravity that attempts to explain the black hole entropy. Using quantum entropy function formalism
we compute logarithmic corrections to the entropy of half BPS black holes in N=2{{\mathcal N}=2} supersymmetric string theories. Our results allow us to test various proposals for the measure in the OSV formula, and we
find agreement with the measure proposed by Denef and Moore if we assume their result to be valid at weak topological string
coupling. Our analysis also gives the logarithmic corrections to the entropy of extremal Reissner–Nordstrom black holes in
ordinary Einstein–Maxwell theory. 相似文献
16.
从Reissner-Nordstrom时空背景下的Klein-Gordon方程出发,利用改进的brick-wall方法膜模型,计算黑洞背景下标量场的自由能和熵.得到标量场的熵是由两部分组成的,根据熵是广延量的性质,得到黑洞熵是由两个子热力学系统贡献的.在此基础上给出了新的Bekenstein-Smarr公式.结果表明,用两个子热力学系统表达的熵,当黑洞的辐射温度趋于绝对零度时,黑洞的熵也趋于零,它满足能斯特定理,可视为黑洞的普朗克绝对熵.
关键词:
brick-wall方法
膜模型
黑洞熵
能斯特定理 相似文献
17.
Taking into account the effect of the generalized uncertainty principle on the generalized black hole entropy and tacking the thin film brick-wall model, we calculate the entropy of the quantum scalar field in generalized static black hole. The Bekenstein–Hawking entropies of all well-known static black holes are obtained. The entropy of 2-D membrane just at the event horizon of static black hole is also calculated, and the result of the black hole entropy proportional to the event horizon area can be obtained more easily and generally. This discussion shows that black hole entropy is just identified with the entropy of the quantum field on the event horizon. The difference from the original brick-wall model is that the present result is convergent without any cutoff and the little mass approximation is removed. With residue theorem, the integral difficulty in the calculation of black hole entropy is overcome. 相似文献
18.
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
19.
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
20.
Considering the unfixed background space-time and self-gravitational interaction, we view the Hawking radiation of a stationary
Kerr–Newman black hole by Hamilton–Jacobi method. Meanwhile, extending this work to non-stationary black holes, we attempt
to investigate the Hawking radiation of the non-stationary Kerr–Newman black hole. Both of the results show the tunneling
probabilities are related to the change of Bekenstein- Hawking entropy and the radiation spectrums deviate from the purely
thermal one, which is in accordance with the known result. 相似文献