共查询到19条相似文献,搜索用时 171 毫秒
1.
利用黑洞的绝热不变性,研究了引力彩虹时空中Kerr黑洞的熵谱和面积谱.首先,在引力彩虹时空背景下,计算了Kerr黑洞的绝热不变作用量,并将其与玻尔-索末菲量子化条件相结合,给出了黑洞的熵谱.得到的熵谱没有引力彩虹时空本身具有的粒子能量依赖性,且是与经典Kerr黑洞中原始贝肯斯坦熵谱相同的等间距熵谱.然后,根据黑洞热力学第一定律和黑洞熵谱,给出了与原始贝肯斯坦谱不同的面积谱.该面积谱是非等间距的,而且有对黑洞面积的依赖性,但不依赖于探测粒子的能量.面积谱表明,随着黑洞面积的减少,面积间隔逐步变小;当黑洞达到普朗克尺度时,面积量子可降为零.这表示黑洞面积不再减少,黑洞出现辐射剩余.而在忽略色散关系的修正效应或在大黑洞极限下,面积谱的修正项可以忽略,引力彩虹Kerr黑洞面积谱可以回归到原始贝肯斯坦谱.此外,对引力彩虹时空Kerr黑洞的熵进行了讨论,得到了带有面积倒数修正项的黑洞熵,分析了黑洞熵的量子修正与面积谱量子修正的一致性. 相似文献
2.
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
3.
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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通过应用在量子引力中,由广义测不准关系得出的新的态密度方程,研究三维BTZ背景下黑洞的熵.当取广义测不准关系中引入的,具有Planck量级与空间维数有关的常数λ为特定值时,得到BTZ黑洞Bekenstein-Hawking 熵和修正项.由于利用新的态密度方程,在计算中不存在用brick-wall模型计算黑洞熵时出现的发散项和小质量近似.所得结论,从量子统计力学角度给出了黑洞Bekenstein-Hawking 熵的修正值,使人们对黑洞熵的修正值有更深入的认识.
关键词:
广义测不准关系
量子统计
BTZ黑洞熵 相似文献
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Parikh最近将黑洞辐射视为半经典的隧穿过程,在考虑了自引力相互作用后,得出静态球对称Schwarzschild和Reissner-Nordstrm黑洞的辐射谱不是纯热谱.采用Doran给出的Kerr黑洞解的新形式,将Parikh的工作推广到Kerr黑洞,研究转动黑洞的隧穿辐射,得到了修正的辐射谱,它与黑洞的Bekenstein-Hawking熵变有关,不是纯热谱,但满足量子力学中的幺正性原理.
关键词:
Kerr黑洞
隧穿辐射
自引力修正
Bekenstein-Hawking熵 相似文献
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11.
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
12.
In this paper we consider 2D Maxwell-dilaton gravity and calculate modified entropy due to higher order terms of the form
∑a
n
R
n
. We find that, higher order correction decreases the value of the black hole entropy. Then we compare the effect of higher
order corrections with effect of Chern-Simons term on the black hole entropy and obtain the expansion coefficient a
n
. 相似文献
13.
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
14.
Fan Zhao 《International Journal of Theoretical Physics》2011,50(11):3509-3514
Taking WKB approximation to solve the scalar field equation in the Schwarzschild black hole spacetime, we can get the classical
momenta. Substituting the classical momenta into state density equation corrected by the modified dispersion relation, we
will obtain the number of quantum states with energy less than ω. Then, it is used to calculate the statistical-mechanical entropy of the scalar field in the Schwarzschild black hole spacetime.
By taking exact method, we obtained the leader term of entropy which is proportional to the event horizon area and correction
terms take the forms of ln A, A
−1ln A, A
−1 and so on. 相似文献
15.
《Nuclear Physics B》1995,451(3):677-695
We discuss the most general effective Lagrangian obtained from the assumption that the degrees of freedom to be quantized, in a black hole, are on the horizon. The effective Lagrangian depends only on the induced metric and the extrinsic curvature of the (fluctuating) horizon, and the possible operators can be arranged in an expansion in powers of MP1/M, where MP1 is the Planck mass and M the black hole mass. We perform a semiclassical expansion of the action with a formalism which preserves general covariance explicitly. Quantum fluctuations over the classical solutions are described by a single scalar field living in the (2 + 1)-dimensional world-volume swept by the horizon, with a given coupling to the background geometry. We discuss the resulting field theory and we compute the black hole entropy with our formalism. 相似文献
16.
Naresh Dadhich Josep M. Pons Kartik Prabhu 《General Relativity and Gravitation》2012,44(10):2595-2601
The necessary and sufficient condition for the thermodynamical universality of the static spherically symmetric Lovelock black hole is that it is the Nth order pure Lovelock Λ-vacuum solution. By universality we mean the thermodynamical parameters: temperature and entropy always bear the same relation to the horizon radius for d = 2N + 1, 2N + 2 dimensions for all N which is the degree of the Lovelock polynomial. For instance, the entropy always goes in terms of the horizon radius as r h and r h 2, respectively for the odd and even dimensions. Not only that the universality uniquely identifies the pure Lovelock black hole with Λ, it is the characterizing property of this class of black holes. 相似文献
17.
We investigate the attractor mechanism in a Kaluza–Klein black hole solution in the presence of higher derivative terms. In
particular, we discuss the attractor behavior of static black holes by using the effective potential approach as well as the
entropy function formalism. We consider different higher derivative terms with a general coupling to the moduli field. For
the R
2 theory, we use an effective potential approach, looking for solutions which are analytic near the horizon and showing that
they exist and enjoy attractor behavior. The attractor point is determined by extremization of the modified effective potential
at the horizon. We study the effect of the general higher derivative corrections of R
n
terms. Using the entropy function we define the modified effective potential and we find the conditions to have the attractor
solution. In particular for a single charged Kaluza–Klein black hole solution we show that a higher derivative correction
dresses the singularity for an appropriate coupling, and we can find the attractor solution. 相似文献
18.
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
19.
Parthasarathi Majumdar 《Pramana》2000,55(4):511-527
This survey intends to cover recent approaches to black hole entropy which attempt to go beyond the standard semiclassical
perspective. Quantum corrections to the semiclassical Bekenstein-Hawking area law for black hole entropy, obtained within
the quantum geometry framework, are treated in some detail. Their ramification for the holographic entropy bound for bounded
stationary spacetimes is discussed. Four dimensional supersymmetric extremal black holes in string-based N=2 supergravity are also discussed, albeit more briefly. 相似文献