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     

环面黑洞背景下量子场的熵

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     

Gibbons-Maeda dilaton 黑洞的纠缠熵

按纠缠熵方法，计算了Gibbons-Maeda(G-M)dilaton黑洞视界外部与黑洞内量子态纠缠的一薄层内量子场的统计熵，得到了G-M dilaton黑洞的Bekenstein-Hawking熵.用广义不确定原理对量子态密度进行修正，克服了brick-wall模型中视界附近态密度的发散困难，该薄层可以紧贴在事件视界上.对brick-wall外部量子场中与黑洞内自由度有关联的自由度统计熵进行了计算，并把结果与brick-wall内量子场的熵进行比较分析，显示两结果具有与视界面积成正比的一致性，但后者能更 关键词： 纠缠熵 黑洞 广义不确定原理 截断     

动态广义球对称含荷黑洞Dirac场的熵

利用改进后的薄膜brick-wall模型，计算了动态广义球对称含荷黑洞Dirac场的熵.按薄层模型的观点，在视界附近薄场上的熵就是黑洞的熵.计算结果表明所得到的黑洞熵与其视界面积成正比. 关键词： 黑洞 薄膜brick-wall模型 熵 Dirac场     

一般球对称带电蒸发黑洞Dirac场的熵

采用薄层模型brick-wall方法，计算了一般球对称带电蒸发黑洞Dirac场的熵，通过适当选择时间依赖的截断因子，仍可得出黑洞熵与视界面积成正比的结论. 关键词： 熵 蒸发黑洞 薄层模型 Dirac场 Dirac方程     

Anti-de Sitter时空中黑洞量子熵的发散结构

用“brick- wall”模型研究了Anti-de Sitter时空中起源于电磁和引力场的黑洞量子熵的发散结构, 结果表明量子熵由线性发散项和对数发散项构成. 如果平衡温度选为Hawking温度，固有截断替代坐标截断，则线性发散项可化为正比于事件视界面积的形式；而对数发散项不仅依赖于黑洞的特征，也依赖于场的自旋，由于此项的存在，自旋场的贡献不再与标量场的贡献成正比. 关键词： 发散结构 黑洞熵 AdS时空 电磁和引力场     

球对称动态黑洞Dirac场的统计熵

利用改进的brick-wall模型，计算最一般球对称动态黑洞Dirac场的统计熵.结果表明，任一时刻黑洞熵都与黑洞事件视界面积成正比.特别是给出了动比例系数的计算公式，通过计算动比例系数，可直接得出各种球对称动态黑洞Dirac场的统计熵. 关键词： 事件视界 黑洞熵 Dirac场 动比例系数     

广义不确定关系与整体单极黑洞Dirac场的熵

将广义不确定关系引入新的态密度方程，采用WKB近似方法，对含整体单极黑洞Dirac场的熵进行了直接计算，所得黑洞熵与它的视界面积成正比，以此揭示了黑洞熵是其视界面处量子态的熵.与brick-wall模型方法不同，该结果不需要取任何截断.同时表明，用此方法不仅可以计算黑洞标量场的熵，而且可以计算Dirac场的熵.     

Schwarzschild黑洞背景下Dirac场的熵

利用brick-wall方法计算了Schwarzschild黑洞背景下Dirac场的自由能和熵,得出了Dirac场的熵与黑洞视界面积成正比的结论,并进一步指出了Schwarzschild黑洞背景下Dirac场的熵为相应Klein-Gordon场的熵的7/2倍- 关键词：     

Quantum entropy of Dirac field in toroidal black hole

The quantum entropy of Dirac field in toroidal black hole is considered and the effects of the spins of the Dirac particles on the entropy are investigated using brick-wall model. It is shown that the quantum entropy has both linearly and logarithmically divergent terms and it has the different structure from that of the black hole. It is also shown that the contribution of the subleading logarithmic term which relates to the spins of the Dirac particles are always positive.     

Statistical Entropy of Horowitz—Strominger Black Hole

The partition functions of bosonic and fermionic fields in Horowitz-Strominger black hole are derived directly by quantum statistical method.Then via the improved brick-wall method (membrane model),the statistical entropy of black hole is obtained.If a proper parameter is chosen in our result,it is found out that the entropy is proportional to the area of horizon.The stripped term and the divergent logarithmic term in the original brick-wall method no longer exist.The difficulty in solving the wave equations of scalar and Dirac fields is avoided.A new neat way of calculating the entropy of various complicated black holes is offered.     

Quantum Corrections to the Entropy of a Black Hole with a Global Monopole

Quantum corrections to the entropy of a static, spherically symmetric blackhole—global monopole system arising from the Dirac spinor field are investigatedby using the brick wall method. It is shown that if we ignore the usual contributionfrom the vacuum surrounding the system, then the quantum corrections for thestatic black hole consist of two parts: One is a quadratically divergent term whichtakes a geometric character. The other is a logarithmically divergent term whichis not proportional to the area of the horizon. The renormalization of the quadraticand logarithmic divergences is also investigated.     

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.     

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.     

Letter: Quantum Statistical Entropy of d-Dimensional Horowitz–Strominger Black Hole

By using the method of quantum statistics, we derive directly the partition functions of bosonic and fermionic field in the d-dimensional Horowitz-Strominger black hole. The statistical entropy of black hole is obtained by an improved brick—wall method. When we choose proper parameter in our results, we can obtain that the entropy of the black hole is proportional to the area of the horizon. In our result, there don't exist the left out term and divergent logarithmic term given in the original brick—wall method. We avoid the difficulty in solving the wave equation of scalar and Dirac field. And we offer a simple and direct way of studying entropy of the higher-dimensional complicated black hole.     

Generalized Uncertainty Principle and Black Hole Entropy of Higher-Dimensional de Sitter Spacetime

Recently, there has been much attention devoted to resolving the quantum corrections to the Bekenstein-- Hawking black hole entropy. In particular, many researchers have expressed a vested interest in the coetticient of the logarithmic term of the black hole entropy correction term. In this paper, we calculate the correction value of the black hole entropy by utilizing the generalized uncertainty prlnciple and obtain the correction term caused by the generalized uncertainty principle. Because in our calculation we think that the Bekenstein-Hawking area theorem is still valid after considering the generalized uncertainty principle, we derive that the coefficient of the logarithmic term of the black hole entropy correction term is positive. This result is different from the known result at present. Our method is valid not only for four-dimensional spacetimes but also for higher-dimensional spacetimes. In the whole process, the physics idea is clear and calculation is simple. It offers a new way for studying the entropy correction of the complicated spacetime.     

Generalized Uncertainty Principle and Correction Value to the Kerr Black Hole Entropy

Recently, there has been much attention devoted to resolving the quantum corrections to the Bekenstein-Hawking black hole entropy. In particular, many researchers have expressed a vested interest in the coefficient of the logarithmic term of the black hole entropy correction term. In this paper, we calculate the correction value of the black hole entropy by utilizing the generalized uncertainty principle and obtain the correction term caused by the generalized uncertainty principle. Because in our calculation we think that the Bekenstein-Hawking area theorem is still valid after considering the generalized uncertainty principle, we derive that the coefficient of the logarithmic term of the black hole entropy correction term is positive. This result is different from the known result at present. Our method is valid not only for single horizon spacetime but also for spin axial symmetric spacetimes with double horizons. In the whole process, the physics idea is clear and calculation is simple. It offers a new way for studying the entropy correction of the complicated spacetime.     

Generalized Uncertainty Principle and Black Hole Entropy of Higher-Dimensional de Sitter Spacetime

Recently, there has been much attention devoted to resolving the quantum corrections to the BekensteinHawking black hole entropy. In particular, many researchers have expressed a vested interest in the coefficient of the logarithmic term of the black hole entropy correction term. In this paper, we calculate the correction value of the black hole entropy by utilizing the generalized uncertainty principle and obtain the correction term caused by the generalized uncertainty principle. Because in our calculation we think that the Bekenstein-Hawking area theorem is still valid after considering the generalized uncertainty principle, we derive that the coefficient of the logarithmic term of the black hole entropy correction term is positive. This result is different from the known result at present. Our method is valid not only for four-dimensional spacetimes but also for higher-dimensional spacetimes. In the whole process, the physics idea is clear and calculation is simple. It offers a new way for studying the entropy correction of the complicated spacetime.     

Nernst Theorem and Statistical Entropy of 5-Dimensional Rotating Black Hole

In this paper, by using quantum statistical method, we obtain the partition function of Bose field and Fermi field on the background of the 5-dimensional rotating black hole. Then via the improved brick-wall method and membrane model, we calculate the entropy of Bose field and Fermi field of the black hole. And it is obtained that the entropy of the black hole is not only related to the area of the outer horizon but also is the function of inner horizon‘s area. In our results, there are not the left out term and the divergent logarithmic term in the original brick-wall method.The doubt that why the entropy of the scalar or Dirac field outside the event horizon is the entropy of the black hole in the original brick-wall method does not exist. The influence of spinning degeneracy of particles on entropy of the black hole is also given. It is shown that the entropy determined by the areas of the inner and outer horizons will approach zero,when the radiation temperature of the black hole approaches absolute zero. It satisfies Nernst theorem. The entropy can be taken as the Planck absolute entropy. We provide a way to study higher dimensional black hole.