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     

变加速直线运动黑洞的温度和Dirac场的熵

采用Tortoise坐标变换,约化视界面附近Dirac场方程,得到Kinnersley黑洞的Hawking温度.用薄膜brick-wall模型,计算Kinnersley黑洞的熵,得到通过选择适当的截断因子和薄层,在视界面附近薄层上的熵就是黑洞的熵,结果表明黑洞熵与视界面积成正比.     

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     

球对称动态黑洞Dirac场的熵的再讨论

采用新的广义乌龟坐标变换,利用薄膜brick-wall模型.讨论了球对称动态黑洞Driac场的Hawking温度和熵,由于k因子的变化,使Hawking温度有一定影响,而截断因子不再因时空结构不同而异,变得与稳态情况相同.关键词：广义乌龟坐标变换薄膜brick-wall模型Driac场熵     

一般加速带电带磁的动态黑洞中标量场的熵

在一般加速带电带磁的动态黑洞中,化简Klein-Gordon场方程,利用乌龟坐标变换,得到在视界面附近的辐射温度.用薄膜brick-wall模型,选择适当的截断因子和薄膜厚度,得到在视界面附近薄膜上的熵,结果表明黑洞熵与视界面积成正比.关键词：黑洞Hawking温度薄膜brick-wall模型熵     

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     

Gibbons-Maeda dilaton黑洞的全息熵

依据全息原理,通过计算Gibbons-Maeda dilaton黑洞事件视界上量子场的统计熵,得到了该黑洞的全息熵和Bekenstein-Hawking熵.计算中利用非对易量子场论,克服了普通量子场论中态密度在视界上的发散困难,避免了黑洞熵热气体方法中紫外截断的引入.用留数定理克服了计算中的积分困难,所得的结果定量成立.研究表明,黑洞熵可以视为其视界上量子场的熵;通过计算视界上量子态的统计熵可以得到黑洞熵,计算中可以且应该避免视界外量子态的影响.关键词：黑洞熵全息原理事件视界非对易量子场论     

起源于引力场的Vaidya-Bonner-de Sitter黑洞的量子熵

利用brick-wall模型研究了引力场对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-Nordstrm-de Sitter黑洞的量子熵完全相 同.     

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：     

Discussion of Garfinkle-Horowitz-Strominger Dilaton Black Hole Entropy

We discuss the entropy of the Garfinkle-Horowitz-Strominger dilaton black hole by using the thin film brick-wall model, and the entropy obtained is proportional to the horizon area of the black hole confirming the Bekenstein-Hawking＇s area-entropy formula. Then, by comparing with the original brick-wall method, we find that the result obtained by the thin film method is more reasonable avoiding some drawbacks, such as little mass approximation, neglecting logarithm term, and taking the term L^3 as a contribution of the vacuum surrounding the black hole, and the physical meaning of the entropy is more clearer.     

Discussion of Garfinkle-Horowitz-Strominger Dilaton Black Hole Entropy

We discuss the entropy of the Garfinkle-Horowitz-Strominger dilaton black hole by using the thin film brick-wall model, and the entropy obtained is proportional to the horizon area of the black hole confirming the Bekenstein-Hawking's area-entropy formula. Then, by comparing with the original brick-wall method, we find that theresult obtained by the thin film method is more reasonable avoiding some drawbacks, such as little mass approximation, neglecting logarithm term, and taking the term L³ as a contribution of the vacuum surrounding the black hole, and the physical meaning of the entropy is more clearer.     

Entropy of charged dilaton-axion black hole with minimal length revisited

Using the generalized uncertainty principle, we calculate the entropy of the charged dilaton-axion black hole for both asymptotically flat and non-flat cases by counting degrees of freedom near the horizon. The divergence of density of states and free energy appearing in the thin film brick-wall model is removed without any cutoff. The entropy proportional to the horizon area is derived from the contribution of the vicinity of the horizon.      

Entropy of quantum field in toroidal black hole without brick wall

In this paper the entropy of a toroidal black hole due to a scalar field is investigated by using the DLM scheme. The entropy is renormalized to the standard Bekenstein-Hawking formula with a one-loop correction arising from the higher curvature terms of the gravitational action. For the scalar field, the renormalized Newton constant and two renormalized coupling constants in the toroidal black hole are the same as those in the Reissner-Nordstrom black hole except for other one.     

Rediscussion of charged dilaton-axion black hole entropy

We rediscuss the entropy of a charged dilaton-axion black hole for both the asymptotically flat and non-flat cases by using the thin film brick-wall model. This improved method avoids some drawbacks in the original brick-wall method such as the small mass approximation, neglecting the logarithm term, and taking the term L ³ as the contribution of the vacuum surrounding the black hole. The entropy we obtain turns out to be proportional to the horizon area of the black hole, conforming to the Bekenstein-Hawking area-entropy formula for black holes.      

Entropy of a Uniformly Accelerating Black Hole

Kinnersley has discussed the space–time of an arbitrarily accelerating point mass. We select a simple case in which the black hole is uniformly accelerated and the mass does not vary with time. We adopt thin film brick-wall model to calculate the entropy of black hole. We find that both the temperature and the entropy density of black hole can be calculated at every point on the horizon. This result indicates that the conclusion that black hole entropy is proportional to its area can be applied to horizon not only globally, but also locally.     

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.     

Entropy and topology of the Kerr—de Sitter black hole

By using the path integral method of Gibbons and Hawking, the entropy of the Kerr-de Sitter black hole is investigated under the microcanonical ensemble. We find that the entropy is one eighth the sum of the products of the Euler number of its cosmological horizon and event horizon with their respective areas. It is shown that the origin of the entropy of the black hole is related to the topology of its instanton.     

Entropy of Gibbons—Maeda 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 Gibbons—Maeda dilation black hole due to arbitrary spin fields. The result shows that the entropy of a scalar field and the entropy of a fermion field have similar formulas. There is only a coefficient difference between them. Furthermore, both entropies depend on the degeneracy of the field.     

The Free Energy and Entropy of Schwarzschild Black Hole Due to Scalar Field

Using the thin film brick-wall model,taking into account the effect of the generalized uncertainty principle on the equation of the density of the states, we calculate the free energy and entropy of schwarzschild black hole due to scalar field, we obtain the entropy proportional to the event horizon area without cutoff. This implies that quantum theory of gravity can remove the divergence of the state density on the event horizon and avoid the cutoff in the original brick-wall model, these results also mean that the thin film brick-wall model is universal. PACS: 0420;9760L.