Kerr-Newman-de Sitter黑洞的统计熵

避开求解波动方程的困难，利用量子统计的方法，直接计算Kerr-Newman-de Sitter黑洞背景下玻色场和费米场的配分函数.然后利用砖墙膜模型计算和讨论黑洞背景下的玻色场和 费米场的熵. 关键词： 量子统计 砖墙膜模型 Kerr-Newman-de Sitter黑洞 统计熵     

Barriola-Viienkin黑洞的统计熵

利用量子统计方法,直接计算Barriola-Vilenkin黑洞背景下玻色场和费米场的配分函数,然后利用砖墙膜模型计算和讨论黑洞背景下玻色场和费米场的熵.     

Barriola-Vilenkin黑洞的统计熵

利用量子统计方法 ,直接计算Barriola_Vilenkin黑洞背景下玻色场和费米场的配分函数 ,然后利用砖墙膜模型计算和讨论黑洞背景下玻色场和费米场的熵     

Kerr 时空黑洞熵和测不准关系

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,直接求解轴对称Kerr黑洞背景下Bose场和Fermi场的配分函数.然后,在黑洞视界附近计算黑洞背景下Bose场和Fermi场的熵.在所得结论中不存在用brick wall模型计算黑洞熵时出现的发散项,也不存在紫外因子.得到黑洞熵与视界面积成正比的结论.     

广义测不准关系与三维BTZ黑洞熵

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     

平面对称黑洞的统计熵

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,计算平面对称黑面背景下玻色场与费米场的配分函数,得到黑面熵的积分表达式.然后应用改进的brickwall方法膜模型,计算黑面视界所对应的统计熵.在所得结果中当所取的积分下限和上限都趋于视界上时,可得到黑面熵与相应黑面视界面积成正比的关系,不存在原brickwall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,为研究黑洞熵提供了一条简捷的新途径 关键词： 量子统计 膜模型 黑面熵     

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     

黑洞熵无截断薄层模型的改进与推广

将广义测不准关系引入薄层brick wall模型，撇开截断因子计算黑洞熵的方法于2002年首次 提出.当时这个方法尚存在一些问题，只得到了熵的上限与视界面积成正比.对这个方法做了些改进，得到熵与视界面积成正比的结果，并讨论了比例因子与广义测不准关系中二阶项待定系数的关系.然后把这种方法推广到非球对称的Rindler视界，得到了预期的结果.揭示了黑洞熵与引力场量子化之间的关系. 关键词： 广义测不准关系 黑洞 熵 Rindler视界     

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     

Einstein-Bumblebee引力理论中的Kerr-Sen-like黑洞玻色子隧穿辐射

Lorentz-breaking理论不仅对弯曲时空背景有影响,而且对于在弯曲时空中的玻色子和费米子的动力学方程都有一定的修正.因此,我们需要在不同的黑洞时空中对玻色子和费米子的量子隧穿辐射进行适当的修正.从而得到经过Lorentz-breaking理论修正后的黑洞Hawking温度等物理量的新表达式及其物理意义.本文根据Einstein-Bumblebee引力理论中得到的Kerr-Sen-like (KSL)黑洞时空度规,在标量场作用量中引入aether-like场矢量修正项和弯曲时空中的d’Alembert算符并应用弯曲时空中的变分原理,研究了此时空度规中的Lorentz-breaking修正项及KSL时空中自旋为零的含有Lorentz-breaking修正项的玻色子动力学方程的新形式.通过正确选择与KSL时空度规相对应的aether-like场矢量,求解修正的玻色子动力学方程,得到了修正的量子隧穿率,并在此基础上研究了含有Lorentz-breaking修正项的此黑洞的Hawking温度和Bekenstein-Hawking熵.此外,还研究了Lorentz-breaking效应对玻...     

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.     

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.     

Bekenstein-Hawking Cosmological Entropy and Correction Term Corresponding Cosmological Horizon of Rotating and Charged Black String

Utilizing the quantum statistical method and applying the new state density equation motivated by generalized uncertainty principle in quantum gravitaty, we avoid the difficulty in solving wave equation and directly calculate the partition function ofbosonic and fermionic field on the background of rotating and charged black string. Then near the cosmological horizon, entropies of bosonic and fermionic field are calculated on the background of black string. When constant λ introduced ingeneralized uncertainty principle takes a proper value, we derive Bekenstein-Hawking entropy and the correction value corresponding cosmological horizon on the background of rotating and charged black string. Because we use the new state density equation, in our calculation there are not divergent term and small massapproximation in the original brick-wall method. From the view of quantum statistic mechanics, the correction value to Bekenstein-Hawking entropy of the black string is derived. It makes people deeply understand the correction value to the entropyof the black string cosmological horizon in non-spherical coordinate spacetime.     

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     

Kaluza—Klein Black-Hole Entropy by Quantum Statistics

By using the method of quantum statistics, we directly derive the partition functions of bosonic and fermionic field in Kaluza—Klein black hole with axial symmetry. Then via the improved brick-wall method, membrane model, we obtain that the entropy of bosonic and fermionic field in black hole is proportional to the area of horizon. In our result, the stripped term and the divergent logarithmic term no longer exist. The problem that the state density is divergent around the horizon doesn't exist either. We also give the influence of the spining degeneracy of particles on the entropy of black hole. We offer a new, simple, and direct way of calculating the entropy of different complicated black holes.     

Letter: Dilatonic Black Hole Entropy Without Brick Walls

The properties of the thermal radiation are discussed by using the new equation of state density motivated by the generalized uncertainty relation in the quantum gravity. There is no burst at the last stage of the emission of dilatonic black hole. When the new equation of state density is utilized to investigate the entropy of a bosonic field and fermionic field outside the horizon of a static dilatonic black hole, the divergence appearing in the brick wall model is removed, without any cutoff. It is derived from the contribution of the vicinity of the horizon that the entropy is proportional to the horizon area.     

Quantum Statistical Entropy of Black Hole

By using the method of quantum statistics, we derive the partition function of bosonic and fermionic field in various coordinates and obtain the integral expression of the entropy of a black hole. Then via the improved brick-wall method, membrane model, we obtain that if we choose proper parameter, the entropy of black hole is proportional to the area of horizon. In our result, the stripped term and the divergent logarithmic term in the original brick-wall method no longer exist. We offer a new simple and direct way of calculating the entropy of black holes in various coordinates.     

Entropy of Kerr-Newman Black Hole to All Orders in the Planck Length

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.