黑洞的量子统计熵

避开求解各种粒子波动方程的困难,直接应用量子统计的方法,计算各种坐标描述的黑洞背景下玻色场与费米场的配分函数,得到黑洞熵的积分表达式.然后应用改进的brick wall方法 膜模型,计算黑洞的统计熵.在所得结果中取适当的参数,可得到黑洞熵与视界面积成正比的关系,不存在原brick wall方法中的舍去项与对数发散项.整个计算过程,物理图像清楚,计算简单,为研究各种坐标下黑洞熵提供了一条简捷的新途经.     

自旋场对Barriola-Vilenkin黑洞熵的量子修正

用砖墙模型的方法，讨论了无源电磁、中微子场对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。      

柱黑洞的熵

采用由广义测不准关系得到的新的态密度方程,研究了具有柱对称时空背景下黑柱的熵.利用新的态密度方程后,不通过截断可以消除brick-wall 模型中无法克服的发散项,并且同样可得到黑柱的熵与视界面积成正比的结论.计算结果表明,黑柱熵是视界面上量子态的熵,是一种量子效应,是黑洞的内禀性质.在计算中我们直接应用量子统计的方法,求柱黑洞背景下玻色场与费米场的配分函数,避开了求解各种粒子波动方程的困难,为研究各种时空黑洞熵提供了一条简捷的新途经.     

柱黑洞的熵

采用由广义测不准关系得到的新的态密度方程,研究了具有柱对称时空背景下黑柱的 熵．利用新的态密度方程后,不通过截断可以消除brick-wall模型中无法克服的发散项,并且 同样可得到黑柱的熵与视界面积成正比的结论．计算结果表明,黑柱熵是视界面上量子态的 熵,是一种量子效应,是黑洞的内禀性质．在计算中我们直接应用量子统计的方法,求柱黑洞 背景下玻色场与费米场的配分函数,避开了求解各种粒子波动方程的困难,为研究各种时空黑 洞熵提供了一条简捷的新途经．     

Reissner Nordstrom 黑洞几何中Dirac场的统计熵与能斯特定理

从Reissner Nordstrom时空背景下的 Dirac 方程出发，利用改进的 brick wall 方法-膜模型,计算黑洞背景下Dirac场的自由能和熵.得到Dirac场的熵是由两部分组成的,根据熵是广延量的特性,由此推得作者所讨论的热力学系统应是由两个热力学子系统组成.在此基础上给出了新的Bekenstein Smarr公式.结果表明,作者所定义的熵满足热力学第三定律.可视为黑洞的普朗克绝对熵.     

Vaidya Bonner de Sitter黑洞背景下电磁场的量子熵

在Tortoise坐标系中，利用brick wall模型研究了电磁场对Vaidya Bonner de Sitter黑洞熵的量子修正. 当黑洞事件视界不随超前时间变化时，结果与Reissner Nordstrom de Sitter黑洞的量子熵完全相同.     

Reissner-Nordstrom黑洞几何中Dirac场的统计熵与能斯特定理

从Reissner-Nordstrom时空背景下的Dirac方程出发，利用改进的brick-wall方法-膜模型，计算黑洞背景下Dirac场的自由能和熵，得到Dirac场的熵是由两部分组成的，根据熵是广延量的特性，由此推得作者所讨论了热力学系统应是由两个热力学子系统组成。在此基础上给出了新的Bekenstein-Smarr公式。结果表明，作者所定义的熵满足热力学第三定律。可视为黑洞的普朗克绝对熵。     

非热平衡Schwarzschild de Sitter黑洞的熵

从Schwarzschild de Sitter时空背景下的Klein Gordon方程出发，利用brick wall方法计算了黑洞的自由能和熵。这种黑洞由于存在两个视界面，而且它们的温度不相同，因此用一般方法计算熵存在着一定的困难。采用改进的brick wall模型，认为自由能和熵主要来自于视界附近薄层的贡献，很好地解决了这一困难，并得到了满意的结果。结果表明，这种黑洞的熵为它的两个视界面积之和的1/4，与人们预期的结果相符。由此可见，渐近de Sitter时空中的黑洞熵除了黑洞视界面的贡献之外，还应包括宇宙视界面的贡献。这从一定程度上揭示了黑洞熵与视界面积之间的内在联系，也更进一步地揭示了brick wall模型的本质。     

轴对称Einstein-Maxwell-Dilaton-Axion黑洞熵与能斯特定理

该文利用Ｂｒｉｃｋ Ｗａｌｌ方法，计算轴对称Ｅｉｎｓｔｅｉｎ Ｍａｘｗｅｌｌ Ｄｉｌａｔｏｎ Ａｘｉｏｎ 黑洞背景下标量场的自由能和熵．结果表明，当黑洞具有内外视界时，所得熵不仅与外视界面积有关，而且也是内视界面积的函数．当内视界面积于零时，可回到已知结论．并且表明，用内外视界位置参量表达的熵，在黑洞辐射温度趋于绝对零度时，黑洞的熵也趋于零，它满足能斯特定理，可视为黑洞的普朗克绝对熵．     

A |torus like黑洞熵与能斯特定理

利用 Brick wall 方法,计算非球坐标系,非渐近平直的 torus like 黑洞背景下标量场的自由能和熵. 结果表明，在非渐近平直时空,黑洞具有内外视界时， 所得熵不仅与外视界面积有关，而且也是内视界的函数.进一步证明，用内外视界参量表达的熵，在黑洞辐射温度趋于零时，黑洞的熵也趋于零，它满足能斯特定理，可视为黑洞的普朗克绝对熵.     

Quantum entropy of Dirac fields in black holes

We use the brick-wall model to study the quantum entropy of the Dirac field in a static black hole with a global monopole or a cosmic string. We show that the entropy of the Dirac field contains a quadratically divergent term and two logarithmically divergent ones and it is not proportional to the entropy of the scalar field. The contribution of the logarithmic term to the entropy depends on the black-hole characteristics and is always negative. __________ Translated from Teoreticheskaya i Matematicheskaya Fizika, Vol. 149, No. 1, pp. 60–64, October, 2006.     

The entropy of Garfinkle-Horne dilaton black hole due to arbitrary spin fields

Using the membrane model which is based on brick wall model, we calculated the free energy and entropy of Garfinkle-Horne dilatonic black hole due to arbitrary spin fields. The result shows that the entropy of scalar field and the entropy of Fermionic field have similar formulas. There is only a coefficient between them.     

Thermodynamic quantities around a charged dilaton black hole

We use the brick-wall method to investigate the thermodynamic quantities around a charged dilaton black hole. We show that all the thermodynamic quantities contain two terms: the first term has exactly the same form as in a flat space-time, but the second term depends explicitly on the spin of the fields and therefore cannot be neglected. __________ Translated from Teoreticheskaya i Matematicheskaya Fizika, Vol. 157, No. 1, pp. 154–160, October, 2008.     

Tunneling radiation of a Gibbons-Maeda dilaton black hole

We use the Parikh-Wilczek method to treat Hawking radiation as a tunneling process across the event horizon and calculate the emission rate of a Gibbons-Maeda dilaton black hole. We show that if self-gravitation is taken into account, then the radiation deviates from the purely thermal spectrum, and the corrected spectrum is consistent with an underlying unitary theory. __________ Translated from Teoreticheskaya i Matematicheskaya Fizika, Vol. 151, No. 1, pp. 172–175, April, 2007.     

Hawking radiation of the Kerr-Sen black hole via tunneling

We use the Parikh-Wilczek method to study the Hawking radiation of a Kerr-Sen black hole via tunneling. We show that corrections to the emission rate exist and that the corrected radiation spectrum deviates from the purely thermal spectrum. Our result is consistent with an underlying unitary theory and compatible with earlier results. __________ Translated from Teoreticheskaya i Matematicheskaya Fizika, Vol. 153, No. 3, pp. 358–362, December, 2007.     

Quantum thermal effect of quasi-static evaporating charged black hole

The study of quantum thermal effect of non-static black hole is generalized to the space-time with coordinate (t, r) as variables. Tortoise coordinate equations which are different from not only static space-time but also the non-static space-time described by advanced-Eddington coordinatev have been chosen. Under the condition that the effect of Hawking evaporation is considered, the temperature of black hole and the location of horizon are shown. The results indicate that Hawking radiation temperature can be regarded as a compensating effect under the time-scale transformation. Project supported by the National Natural Science Foundation of China.     

BTZ black hole as a solution of a higher-spin gauge theory in three-dimensional space-time

We show that the BTZ black hole is an exact solution of a higher-spin gauge theory in three-dimensional space-time. We find solutions for free massless fields in the black-hole metric using the star algebra formalism underlying the higher-spin theory. We find that some of the higher-spin symmetries remain unbroken for special values of the BTZ parameters. __________ Translated from Teoreticheskaya i Matematicheskaya Fizika, Vol. 153, No. 2, pp. 158–185, November, 2007.     

Three kinds of horizon-like hypersurface of a uniformly accelerating, non-stationary charged black hole

Three kinds of horizon-like hypersurface of a uniformly rectilinearly accelerating, non-stationary charged black hole: event horizon, apparent horizon and time-like limit surface are studied. The result is that the event horizon is apart from the time-like limit surface and the apparent horizon in the case where the black hole is charged, uniformly accelerating and its mass is varying (evaporating and accreting). Some other new results are also given. Project supported by the National Natural Science Foundation of China.