共查询到19条相似文献,搜索用时 218 毫秒
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引入局域热平衡概念,用Damour-Ruffini方法和薄膜模型研究了缓变动态Kerr-Newman黑洞的Hawking辐射和熵.得到了黑洞的Hawking温度和辐射谱公式,Hawking温度随时间和视界面上的位置而变化,辐射谱为准黑体谱;计算了黑洞熵,当取与静态球对称黑洞情况相同的截断关系时便得到了黑洞的Bekenstein-Hawking熵.结果表明,缓变动态黑洞的温度是局域量,缓变动态黑洞的熵与稳态黑洞情况一样正比于黑洞视界面面积.
关键词:
缓变动态黑洞
Hawking辐射
黑洞熵 相似文献
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在任意加速带电动态时空中,选取零标架、计算出旋系数,把四个耦合的Dirac方程中化成两个耦合的方程,采用Tortoise坐标变换将其两个耦合的方程变换成Tortoise坐标下的形式,在黑洞视界面附近化成了典型的波动方程,得到在视界面附近Dirac粒子的Hawking辐射温度,成功地导出了Hawking热谱公式.
关键词:
Dirac方程
Hawking辐射
黑洞
Tortoise坐标变换 相似文献
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采用Tortoise坐标变换,约化视界面附近Dirac场方程,得到Kinnersley黑洞的Hawking温度.用薄膜brick-wall模型,计算Kinnersley黑洞的熵,得到通过选择适当的截断因子和薄层,在视界面附近薄层上的熵就是黑洞的熵,结果表明黑洞熵与视界面积成正比. 相似文献
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研究了动态Kerr黑洞时空中的粒子能级,计算了最低正能级和最高负能级的精确表达式。在动态Kerr黑洞视界附近的能级交错表明,动态Kerr黑洞的非热辐射的频率范围不仅拖曳角速度有关,而且与黑洞的蒸发率和视界形状也有关。 相似文献
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利用薄层(改进的brick-wall模型),通过分别求解标量场方程和Dirac场方程,计算了环面黑洞事件视界附近的标量场和Dirac场的量子统计熵.按薄层模型的观点,在视界面附近薄层上的量子场的熵就是黑洞的熵.结果表明,黑洞熵正比于事件视界的面积,遵循Beken-stein-Hawking面积熵公式.
关键词:
熵
环面黑洞
薄层模型
量子场 相似文献
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在一般加速带电带磁的动态黑洞中,化简Klein-Gordon场方程,利用乌龟坐标变换,得到在视界面附近的辐射温度.用薄膜brick-wall模型,选择适当的截断因子和薄膜厚度,得到在视界面附近薄膜上的熵,结果表明黑洞熵与视界面积成正比.
关键词:
黑洞
Hawking温度
薄膜brick-wall模型
熵 相似文献
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We first review the accelerating, rotating and charged Plebanski–Demianski (PD) black hole, which includes the Kerr–Newman rotating black hole and the Taub-NUT spacetime. The main feature of this black hole is that it has 4 horizons like event horizon, Cauchy horizon and two accelerating horizons. In the non-extremal case, the surface area, entropy, surface gravity, temperature, angular velocity, Komar energy and irreducible mass on the event horizon and Cauchy horizon are presented for PD black hole. The entropy product, temperature product, Komar energy product and irreducible mass product have been found for event horizon and Cauchy horizon. Also their sums are found for both horizons. All these relations are dependent on the mass of the PD black hole and other parameters. So all the products are not universal for PD black hole. The entropy and area bounds for two horizons have been investigated. Also we found the Christodoulou–Ruffini mass for extremal PD black hole. Finally, using first law of thermodynamics, we also found the Smarr relation for PD black hole. 相似文献
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Deviations from Hawking's thermal black hole spectrum, observable for macroscopic black holes, are derived from a model of a quantum horizon in loop quantum gravity. These arise from additional area eigenstates present in quantum surfaces excluded by the classical isolated horizon boundary conditions. The complete spectrum of area unexpectedly exhibits evenly spaced symmetry. This leads to an enhancement of some spectral lines on top of the thermal spectrum. This can imprint characteristic features into the spectra of black hole systems. It most notably gives the signature of quantum gravity observability in radiation from primordial black holes, and makes it possible to test loop quantum gravity with black holes well above Planck scale. 相似文献
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In this paper, we extend Parikh's recent work to two kinds of the black holes whose ADM mass is no longer identical to its
mass parameter, each with a topological defect, one being a global monopole black hole and another a cosmic string black hole.
We view Hawking radiation as a tunnelling process across the event horizon and calculate the tunnelling probability. From
the tunnelling probability we also find a leading correction to the semiclassical emission rate. The results are consistent
with an underlying unitary theory. 相似文献
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I. B. Khriplovich 《Journal of Experimental and Theoretical Physics》2004,99(3):460-465
An equidistant spectrum of the horizon area of a quantized black hole does not follow from the correspondence principle or from general statistical arguments. On the other hand, such a spectrum obtained in loop quantum gravity (LQG) either does not comply with the holographic bound or requires a special choice of the Barbero-Immirzi parameter for the horizon surface, distinct from its value for other quantized surfaces. The problem of distinguishability of the edges in LQG is discussed, with the following conclusion: Only under the assumption of partial distinguishability of the edges can the microcanonical entropy of a black hole be made both proportional to the horizon area and satisfying the holographic bound. 相似文献
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Poisson E 《Physical review letters》2005,94(16):161103
The metric of a tidally distorted, nonrotating black hole is presented in a light-cone coordinate system that penetrates the event horizon and possesses a clear geometrical meaning. The metric is expressed as an expansion in powers of r/R<1, where r is a measure of distance from the black hole and R is the local radius of curvature of the external spacetime; this is assumed to be much larger than M, the mass of the black hole. The metric is calculated up to a remainder of order (r/R)4, and it depends on a family of tidal gravitational fields which characterize the hole's local environment. The coordinate system allows an easy identification of the event horizon, and expressions are derived for its surface gravity and the rates at which the tidal interaction transfers mass and angular momentum to the black hole. 相似文献
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A new space time metric is derived from Kerr metric if its mass and location approach to infinite in an appropriate way. The new space-time is an infinitesimal neighborhood nearby one of the two horizon poles of an infinite Kerr black hole. In other words, it is the second order infinitesimal neighborhood nearby one of the two horizon poles of a Kerr black hole. It is flat and has event horizon and infinite red shift surface. We prove that it is a rotating Rindler space time with constant angular velocity. 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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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