Anti-de Sitter时空内柱黑洞的量子熵

利用brick-wall方法计算了Anti-de Sitter时空内起源于Dirac场的柱黑洞的量子熵.结果表明，忽略远离围绕系统的真空的贡献时，量子熵包含了线性发散项和对数发散项，整个表达式的形式与标量场的不一样.无论整个对数项还是与自旋联系的子对数项都总是正的. 关键词： brick-wall方法 量子熵 柱黑洞 Dirac场     

自旋场对Barriola-vilenkin黑洞熵的量子修正

用砖墙模型的方法，讨论了无源引力场对Barriola-Vilenkin黑洞熵的量子修正.计算表明， 量子修正应该包含两部分：其中一部分与视界面积成正比，在视界附近与紫外截断因子是 平方反比发散的；另一部分是两个对数发散项，这部分除了与黑洞的本身特征性质(M，η) 有关以外，还与自旋场的自旋有关.结果与标量场引起的量子修正具有完全不同的形式. 关键词： 砖墙模型 量子修正 黑洞熵     

高自旋场对静态球对称黑洞熵的贡献

利用改进后的brick wall模型，研究具有高自旋的引力场对静态球对称黑洞熵的贡献.结果表明：在静态球对称黑洞中，自旋为2的引力场的量子熵仍与视界面积成正比.当选择与标量场相同的截断因子时，其量子熵为标量场的两倍，为Dirac场的4/7. 关键词： 黑洞熵 brick wall模型 自旋场 Teukolsky型主方程     

高自旋场对Vaidya-Bonner黑洞熵的贡献

利用改进的brick-wall模型推导出自旋为2的引力场对动态Vaidya-Bonner 黑洞熵的贡献， 在自然单位制中其值为A/2；这表明，当选择与标量场相同的截断因子时，其熵为标量场的2 倍，为Dirac 场的4/7. 关键词： Vaidya-Bonner黑洞 黑洞熵 高自旋场 薄膜brick-wall模型     

Kerr-Newman黑洞的统计熵

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KerrNewman黑洞背景下Bose场和Fermi场的配分函数.然后利用改进的brickwall方法膜模型,计算黑洞背景下Bose场和Fermi场的熵.得到黑洞熵与视界面积成正比的结论.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.为研究各种复杂黑洞熵提供了简捷的途径. 关键词： 量子统计 brick-wall方法 膜模型 黑洞熵     

Sen黑洞熵与能斯特定理

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     

用砖墙方法和薄层方法计算Gibbons-Maeda黑洞时空中标量场的统计力学熵

利用砖墙方法和薄层方法计算了Gibbons-Maeda黑洞背景时空中标量场的统计力学熵.用砖墙方法求得的统计力学熵有两项:其中一项与Gibbons-Maeda黑洞视界面积成正比,并且当截断因子满足一定的关系时,熵为其视界面积的四分之一;另一项是对数发散项.利用薄层方法所求得的熵只有与Gibbons-Maeda黑洞视界面积成正比的项,对数发散项被自然消去.     

轴对称黑洞的量子统计熵

避开了求解黑洞背景下波动方程的因难,应用量子统计方法,通过应用在量子引力中、由广义测不准关系得出的新态密度方程,直接求解轴对称Kerr黑洞背景下玻色场和费米场的配分函数.然后,在视界附近计算黑洞背景下玻色场和费米场的熵.得到用收敛级数表达的黑洞熵.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,使人们对非球对称时空中黑洞的统计熵有更深入的认识. 关键词： 量子统计 非球对称时空 广义测不准关系 黑洞熵     

球对称动态黑洞的量子能层效应

用Newman-Penrose形式,研究了球对称动态时空中的引力、电磁、标量和Dirac场,表明量子能层会影响动态黑洞的辐射机制.与Kerr能层和电磁势产生的经典效应不同,这个效应的特征是辐射机制明显依赖于自旋态. 关键词：     

黑洞的统计熵

运用量子统计的方法,直接求解Schwarzschild时空背景下玻色场和费米场的配分函数,得到熵的积分表达式.按照最近的研究结果,认为黑洞的Hawking辐射过程是隧道效应过程,在考虑黑洞隧道效应产生过程中黑洞能量发生变化的基础上,给出积分的下限为黑洞的视界位置.由此得到黑洞熵的主要项为视界面积的1/4.不存在使人疑惑的紫外截断因子,并且由此可得黑洞辐射粒子的能量与辐射温度成正比的结论. 关键词： 黑洞熵 量子统计 隧道效应 反作用     

Calculating Entropy of Plane Symmetry Black Hole via Generalized Uncertainty Relation

The generalized uncertainty relation is introduced to calculate entropy of the black hole. By using quantum statistical method, we directly obtain the partition function of Bose and Fermi field on the background of the plane symmetry black hole. Then we calculate the entropy of Bose and Fermi field on the background of black hole near the horizon of the black hole. In our calculation, we need not introduce cutoff. There are not the left out term and the divergent logarithmic term in the original brick-wall method. And it is obtained that the entropy of the black hole is proportional to the area of the horizon. The inherent contact between the entropy of black hole and the area of horizon is opened out. Further it is shown the entropy of black hole is 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.     

Quantum Statistical Entropy of Five-Dimensional Black Hole

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.     

Entropy of N-Dimensional Spherically Symmetric Charged Black Hole

By using the method of quantum statistics, we derive directly the partition functions of bosonic andfermionic fields in the N-dimensional spherically symmetric charged black hole space-time. The statistical entropy ofblack hole is obtained by an improved brick-wall method. When we choose proper parameters in our results, we canobtain that the entropy of black hole is proportional to the area of horizon. In our result, there do not exist neglectedterm and divergent logarithmic term given in the original brick-wall method. We avoid the difficulty in solving the waveequation of scalar and Dirac fields. We offer a simple and direct way of studying entropy of the higher-dimensional black hole.     

Entropy of the Quantum Scalar Field in Static Black Holes

The quantum corrections to the entropy of staticblack holes are investigated by two methods: the brickwall method of 't Hooft and the Euclidean path integralapproach of Gibbons and Hawking. Two general formulas for the entropy are obtained and someexamples are considered. It is shown that if thecontribution from the vacuum surrounding the system isignored, then the two approaches give the same results. It is found that the entropy of the quantumscalar field in a general static black hole consists oftwo parts: a quadratically divergent term which takes ageometric character and a logarithmically divergent term which is not proportional to the horizonarea. The logarithmically divergent term, in general,depends on the black hole characteristics (inparticular, the whole entropy is determined only by this term for some extreme cases) and thereforecannot be neglected as a nonessential additive constant.The renormalization of the entropy is also discussedbriefly.     

Divergence structure of the statistical entropy of the Dirac field in a plane symmetry black hole geometry

The divergences at all levels for the statistical entropy of a plane symmetry black hole arising from the massless Dirac field are considered using the brick-wall model. It is shown that if we ignore the usual contribution from the vacuum surrounding the system, then the statistical entropy consists of two parts: one is the linearly divergent term which has the geometric character, the other consists of two logarithmically divergent terms which are not proportional to the surface area of the horizon. The entropy of the Dirac field on extremal plane symmetry spacetime background has higher divergence than usual.     

Quantum Entropy of Spin Fields in the Schwarzschild-Anti-de Sitter Black Hole with a Global Monopole

The quantum entropies of gravitational, electromagnetic, neutrino and scalar fields in the static Schwarzschild-anti-de Sitter black hole with a global monopole are investigated by using the brick-wall model. The quantum entropy contain two parts: One is quadratically divergent term which takes a geometric character; the other is spin-dependent, logarithmically divergent terms. The whole expression of the entropy of a spin field does not take the form of the scalar field. PACS: 04.70. Dy, 97.60.Lf     

Entropy of Reissner—Nordstrom—De Sitter Black Hole in Nonthermal Equilibrium

By making use of the method of quantum statistics,we directly derive the partition function of bosonic and fermionic fields in Reissner-Nordstrom-De Sitter black Hole and obtain the integral expression of black hole‘s entropy and the entropy to which the cosmic horizon surface corresponds.It avoids the difficulty in solving the wave equation of various particles.Then via the improved brick-wall method,i.e.the membrane model,we calculate black hole‘s entropy and cosmic entropy and find out that if we let the integral upper limit and lower limit both tend to the horizon,the entropy of black hole is proportional to the area of horizon and the entropy to which cosmic horizon surface corresponds is proportional to the area of cosmic horizon.In our result,the stripped term and the divergent logarithmic term in the original brick-wall method no longer exist.In the whole process,the physical idea is clear and the calculation is simple.We offer a new simple and direct way for calculating the entropy of different complicated black holes.     

Bosonic and fermionic entropy of black holes with different temperatures on horizon surface

By using the method of quantum statistics, we derive directly the partition functions of bosonic and fermionic field in the black hole space－time with different temperatures on horizon surface. The statistical entropy of the black hole is obtained by an improved brick-wall method. When we choose a proper parameter in our results, we can obtain that the entropy of the black hole is proportional to the area of horizon. In our result, there do not exist any neglected term or divergent logarithmic term as given in the original brick-wall method. We have avoided the difficulty in solving the wave equation of the scalar and Dirac field. A simple and direct way of studying entropy of the black hole is given.     

Generalized uncertainty principle and tunnelin gradiation of the SAdS5 black hole

After considering the generalized uncertainty principle, we discuss the quantum tunneling radiation of a five-dimensional Schwarzschild anti de Sitter black hole. The radiation spectrum and the correction value of the Bekenstein-Hawking entropy are derived. In a five-dimensional black hole the one order correction term in the Bekenstein-Hawking entropy correction term is proportional to the third power of the area, and the logarithmic correction term is a two-order small quantity. The correction term is related to the dimension constant introduced in the generalized uncertainty principle. Because the black hole entropy is not divergent, the lowest value of the five-dimensional Schwarzschild anti de Sitter black hole horizon radius is obtained. After considering the generalized uncertainty principle, the radiation spectrum is still consistent with normalization theory.