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Quantum Entropy of Black Hole with Internal Global Monopole 总被引:2,自引:0,他引:2
Using the generalized uncertainty relation, the new equation of state
density is obtained, and then the entropy of black hole with an internal
global monopole is discussed. The divergence that appears in black hole
entropy calculation through original brick-wall model is overcome. The
result of the direct proportion between black hole entropy and its event
horizon area is drawn and given. The result shows that the black hole
entropy must be the entropy of quantum state near the event horizon. 相似文献
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Ren Zhao Li-Chun Zhang Huai-Fan Li Yue-Qin Wu 《International Journal of Theoretical Physics》2008,47(12):3083-3090
Using the quantum statistical method, the difficulty of solving the wave equation on the background of the black hole is avoided.
We directly solve the partition functions of Bose and Fermi field on the background of an axisymmetric Kerr-Newman black hole
using the new equation of state density motivated by the generalized uncertainty principle in the quantum gravity. Then near
the black hole horizon, we calculate entropies of Bose and Fermi field between the black hole horizon surface and the hypersurface
with the same inherent radiation temperature measured by an observer at an infinite distance. In our results there are not
cutoffs and little mass approximation introduced in the conventional brick-wall method. The series expansion of the black
hole entropy is obtained. And this series is convergent. It provides a way for studying the quantum statistical entropy of
a black hole in a non-spherical symmetric spacetime. 相似文献
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利用广义不确定关系修正的态密度方程并采用Wentzel-Kramers-Brillouin (WKB) 近似方法, 计算了Reissner-Nordström-de Sitter (RNdS) 黑洞时空中标量场的统计力学熵. 结果表明, 由这种方法得到的黑洞熵与它的内、外视界面积和宇宙视界面积之和成正比, 这与采用其他方法所得的结果一致, 从而揭示了黑洞熵与视界面积之间的内在联系, 也进一步表明了黑洞熵是视界面上量子态的熵, 是一种量子效应. 相似文献
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Ji-Jian Jiang Yu-Shan Li Jing-Lun Liu Chuan-An Li 《International Journal of Theoretical Physics》2017,56(7):2161-2166
The scatting probability of scalar particles near the event horizon is obtained by solving Klein-Gordon equation in curved space-time. By considering the reaction of a black hole radiation in space-time background, we find that Hawking radiation is not a strictly pure thermal-spectrum and scatting probability is related to the B-H entropy change of black hole. The statistical entropy of black hole is calculated based on the relations between entropy and thermodynamic probability of a macroscopic state in statistical equilibrium. The results show that the statistical entropy of black hole without using any truncation factor is proportional to the area of event horizon. 相似文献
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利用广义不确定关系修正的态密度方程并采用Wentzel-Kramers-Brillouin(WKB)近似方法,计算了Reissner-Nordstrm-de Sitter(RNdS)黑洞时空中标量场的统计力学熵.结果表明,由这种方法得到的黑洞熵与它的内、外视界面积和宇宙视界面积之和成正比,这与采用其他方法所得的结果一致,从而揭示了黑洞熵与视界面积之间的内在联系,也进一步表明了黑洞熵是视界面上量子态的熵,是一种量子效应. 相似文献
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The properties of the thermal radiation are discussed by using the new equation of state density motivated by the generalized uncertainty relation in the quantum gravity. There is no burst at the last stage of the emission of dilatonic black hole. When the new equation of state density is utilized to investigate the entropy of a bosonic field and fermionic field outside the horizon of a static dilatonic black hole, the divergence appearing in the brick wall model is removed, without any cutoff. It is derived from the contribution of the vicinity of the horizon that the entropy is proportional to the horizon area. 相似文献
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把洛仑兹破缺的标量场方程推广到弯曲时空中,并通过Aether-like项对标量场方程进行修正,该项所产生的效应也会影响到黑洞时空视界附近处的物理效应.接着,进一步在半经典近似下得到了修正的Hamilton-Jacobi方程,然后用这一修正的Hamilton-Jacobi方程研究了史瓦西黑洞的隧穿辐射特征,并讨论了洛仑兹破缺对黑洞霍金辐射和黑洞熵的影响.结果表明,u~α=δ_t~αu~t,δ_r~αu~r形式的Aether-like项的效应可能使黑洞温度增加,而黑洞熵降低.该工作可以帮助我们更深刻地理解弯曲时空中的洛仑兹破缺效应的物理性质. 相似文献
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避开求解黑洞背景下波动方程的困难,应用量子统计方法,直接求解轴对称Sen黑洞背景下Bose场和Fermi场的配分函数.然后利用改进的 brick-wall 方法-膜模型,计算黑洞背景下Bose场和Fermi场的熵.得到黑洞熵不但与黑洞的外视界面积有关,而且也是内视界面积的函数.在所得结论中不存在对数发散项与舍去项,也不存在黑洞视界外标量场或Dirac场为什么是黑洞熵疑难,并且给出粒子的自旋简并度对黑洞熵的影响. 当黑洞的辐射温度趋于绝对零度时,由黑洞内外视界面积决定的黑洞熵也趋于零,它满足能斯特定理,可视
关键词:
膜模型
黑洞熵
能斯特定理 相似文献
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The generalized uncertainty relation is introduced to calculate quantum statistic entropy of a black hole. By using the new equation of state density motivated by the generalized
uncertainty relation, we discuss entropies of Bose field and Fermi
field on the background of the five-dimensional spacetime. In our
calculation, we need not introduce cutoff. There is not the divergent logarithmic term as in the original brick-wall method. And it is obtained that the quantum statistic entropy corresponding to black hole horizon is proportional to the area of the horizon.
Further it is shown that the entropy of black hole is the entropy of
quantum state on the surface of horizon. The black hole's entropy
is the intrinsic property of the black hole. The entropy is a
quantum effect. It makes people further understand the quantum statistic entropy. 相似文献
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Ding-Xiong Wang 《General Relativity and Gravitation》1995,27(12):1251-1258
The entropy of a self-gravitating radiation system (sgrs) confined to a spherical box with a central black hole is calculated by using the equation of state of radiation near a black-hole horizon, which was derived by Li and Liu. The upper bound on the total entropy of the system including the central black hole is exactly equal to the entropy of the black hole with the same mass. A reasonable mode of the gravitational collapse of ansgrs is given, and a possible explanation for the origin of black-hole entropy is provided. 相似文献
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Hawking radiation from the black hole in Ho?ava–Lifshitz gravity is discussed by a reformulation of the tunneling method given in Banerjee and Majhi (2009) [17]. Using a density matrix technique the radiation spectrum is derived which is identical to that of a perfect black body. The temperature obtained here is proportional to the surface gravity of the black hole as occurs in usual Einstein gravity. The entropy is also derived by using the first law of black hole thermodynamics. Finally, the spectrum of entropy/area is obtained. The latter result is also discussed from the viewpoint of quasi-normal modes. Both methods lead to an equispaced entropy spectrum, although the value of the spacing is not the same. On the other hand, since the entropy is not proportional to the horizon area of the black hole, the area spectrum is not equidistant, a finding which also holds for the Einstein–Gauss–Bonnet theory. 相似文献
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Dong-Shan He 《理论物理通讯》2019,71(8):1007-1010
A method for calculating the radiation spectrum of an arbitrary black holes was recently proposed by Ma et al., [Europhys. Lett. 122 (2018) 30001] in which a non-thermal spectrum of a black hole can be obtained from its entropy using an approach based on canonical typicality. The non-thermal spectrum of a black hole enables a nonzero correlation between the black hole and its radiation, which can ensure that information is conserved during black hole evaporation. In this paper, by using the Kantowski-Sachs metric and Feynman-Hibbs procedure, the entropy of a noncommutative quantum black hole is calculated based on the Wheeler-DeWitt equation. Then, the radiation spectrum of the noncommutative quantum black hole is studied based on canonical typicality method. At last, the correlation between the radiation spectra is calculated. It is shown that the noncommutative effect increases the correlation among radiation and the information remains conserved for noncommutative quantum black holes. 相似文献
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Quantum Thermal Effect of Nonstationary Kerr-Newman Black Hole 总被引:4,自引:0,他引:4
The Hawking radiation and the entropy of non-stationary Kerr-Newman black hole whose metric changes slowly are calculated via the method of Damour etc. and the thin film brick-wall model. First, we obtain the Hawking radiation temperature and the thermal spectrum formula. Second, we get the entropy density at every point of the horizon surface as well as the total entropy of the black hole, which is just the Bekenstein-Hawking entropy and relies on the notion of the local equilibrium crucially that can be met if the evaporation and the accretion of the black hole is negligible. The results show that the temperature of the event horizon depends on the time and the angle, and the entropy of the non-stationary black hole is also proportional to the horizon area with appropriate cutoff relationship as in the case of stationary black holes. 相似文献
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The generalized Stefan--Boltzmann law of a rectilinear non-uniformly accelerating Kinnersley black hole 下载免费PDF全文
Using entropy density of Dirac field near the event horizon of a
rectilinear non-uniformly accelerating Kinnersley black hole, the
law for the thermal radiation of black hole is studied and the
instantaneous radiation energy density is obtained. It is found that
the instantaneous radiation energy density of a black hole is always
proportional to the quartic of the temperature on event horizon in
the same direction. That is to say, the thermal radiation of a black
hole always satisfies the generalized Stefan--Boltzmann law. In
addition, the derived generalized Stefan--Boltzmann coefficient is
no longer a constant, but a dynamic coefficient related to the
space--time metric near the event horizon and the changing rate of
the event horizon in black holes. 相似文献