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     

直线加速运动动态黑洞的熵

选取超前爱丁顿坐标,采用薄膜brickwall模型,计算Kinnersley度规表述的直线加速运动动态黑洞的熵.通过此方法,可以给出视界面上每一点的温度和熵密度.这一结果表明,熵与视界面积成正比的结论,不仅适用于整个视界,也适用于视界面上的局部;不仅适用于稳态黑洞,也适用于动态黑洞.在薄膜趋于视界面时,其厚度也趋于零,薄膜本身成为视界面,黑洞熵就是视界面上量子态的熵 关键词： 熵 加速黑洞 薄膜brickwall模型     

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     

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     

动态Dilaton-Maxwell黑洞的广义Stefan-Boltzmann定律

利用动态Dilaton-Maxwell黑洞视界面附近的熵密度,导出黑洞的瞬时辐射流量,得到了任一时刻黑洞沿某一方向的瞬时辐射流量总是正比于在该方向上黑洞事件视界温度的四次方的结论. 导出的广义Stefan-Boltzmann系数不再是一个恒量,而是一个与黑洞视界面附近的时空度规、黑洞视界的变化率及黑洞的吸收与辐射系数有关的动比例系数.揭示了黑洞周围的引力场与其热辐射之间存在着必然的内在联系. 关键词： 熵密度 薄膜模型 瞬时辐射流量 广义Stefan-Boltzmann系数     

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     

直线加速Kinnersley黑洞中Dirac粒子的热辐射

在直线加速Kinnersley时空中,将相互耦合的Dirac方程化为二阶方程,采用新的乌龟坐标变换,在视界面附近消除二阶方程中的耦合化成了标准波动方程,得到辐射温度函数和Hawking热辐射谱. 关键词： 黑洞 Dirac方程 乌龟坐标变换 Hawking辐射     

加速运动动态黑洞的瞬时辐出度

利用加速黑洞视界面附近的熵密度，导出黑洞的瞬时辐出度，得到了任一时刻黑洞沿某一方向的瞬时辐出度总是正比于在该方向上黑洞事件视界温度的四次方的结论. 导出的广义Stefan-Boltzmann系数不再是一个恒量，而是一个与黑洞视界的变化率、黑洞视界面附近的时空度规及黑洞的吸收与辐射系数有关的动比例系数. 揭示了黑洞周围的引力场与其热辐射之间存在着必然的内在联系. 关键词： 薄膜模型 瞬时辐出度 广义Stefan-Boltzmann系数     

变加速直线运动黑洞中Weyl中微子的Hawking辐射

利用推广的乌龟坐标变换法研究了作变加速直线运动的Kinnersley黑洞中Weyl中微子的量子 热效应，导出了局部的事件视界面方程和Hawking温度以及中微子的热辐射谱.结果表明视界 的位置和温度不仅随时间变化，而且明显依赖于方位角. 关键词： Hawking辐射 Weyl中微子 动态Kinnersley黑洞 广义乌龟坐标变换     

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     

Discussing Again on the Thermal Property of Kinnersley Black Hole Using a New Tortoise Coordinate Transformation

By reducing the Klein-Gordon equation near the event horizon with a new tortoise coordinate transformation, we calculate the Hawking temperature of the arbitrarily accelerating Kinnersley black hole. The temperature is a little different from what we have when we select the usual tortoise coordinate transformation. Then by means of the thin film model, we obtain the Bekenstein Hawking entropy of the Kinnersley black hole, which is proportional to the area of its event horizon with the same cut-off relation as the static case.     

The generalized Stefan--Boltzmann law of a rectilinear non-uniformly accelerating Kinnersley black hole

Using entropy density of Dirac field near the event horizon of a rectilinear non-uniformly accelerating Kinnersley black hole, the law for the thermal radiation of black hole is studied and the instantaneous radiation energy density is obtained. It is found that the instantaneous radiation energy density of a black hole is always proportional to the quartic of the temperature on event horizon in the same direction. That is to say, the thermal radiation of a black hole always satisfies the generalized Stefan--Boltzmann law. In addition, the derived generalized Stefan--Boltzmann coefficient is no longer a constant, but a dynamic coefficient related to the space--time metric near the event horizon and the changing rate of the event horizon in 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.     

The Generalized Uncertainty Relation and The Entropy of Non-stationary and Slowly Changing Reissner-Nordstr?m Black Hole

Applying the generalized uncertainty relation to the thin film brick-wall model, the entropy of Dirac Field in Non-stationary and Slowly Changing Reissner-Nordstr?m Black Hole is obtained. The result shows that the entropy is still proportional to the horizon area of the black hole, and black hole entropy is just identical to the entropy of the quantum state near the event horizon, in addition, the divergence of state density without any cut-off parameter is avoided during black hole entropy calculation.     

Radiation Energy Flux and Radiation Power of Schwarzschild Black Hole

Applying the entropy density near the event horizon, we obtained the result that the radiation energy flux of the black hole is always proportional to the quartic of the temperature of its event horizon. That is to say, the thermal radiation of the black hole always satisfies the generalized Stefan–Boltzmann law. The derived generalized Stefan–Boltzmann coefficient is no longer a constant. When the cut-off distance and the thin film thickness are both fixed, it is a proportional coefficient which is related to the black hole mass, the kinds of radiation particles and space–time metric near the event horizon. In this paper, we have put forward a thermal particle model in curved space–time. By this model, the result has been obtained that when the thin film thickness and the cut-off distance are both fixed, the radiation energy flux received by observer far away from the Schwarzschild black hole is proportional to the average radial effusion velocity of the radiation particles in the thin film, and inversely proportional to the square of the distance between the observer and the black hole.     

Black Hole Entropies of the Thin Film Model and the Membrane Model Without Cutoffs

Taking into account the effect of the generalized uncertainty principle on the generalized black hole entropy and tacking the thin film brick-wall model, we calculate the entropy of the quantum scalar field in generalized static black hole. The Bekenstein–Hawking entropies of all well-known static black holes are obtained. The entropy of 2-D membrane just at the event horizon of static black hole is also calculated, and the result of the black hole entropy proportional to the event horizon area can be obtained more easily and generally. This discussion shows that black hole entropy is just identified with the entropy of the quantum field on the event horizon. The difference from the original brick-wall model is that the present result is convergent without any cutoff and the little mass approximation is removed. With residue theorem, the integral difficulty in the calculation of black hole entropy is overcome.     

Radiation energy flux of Dirac field of static spherically symmetric black holes

By the statistical entropy of the Dirac field of the static spherically symmetric black hole, the result is obtained that the radiation energy flux of the black hole is proportional to the quartic of the temperature of its event horizon. That is, the thermal radiation of the black hole always satisfies the generalised Stenfan--Boltzmann law. The derived generalised Stenfan--Boltzmann coefficient is no longer a constant. When the cut-off distance and the thin film thickness are both fixed, it is a proportional coefficient related to the space--time metric near the event horizon and the average radial effusion velocity of the radiation particles from the thin film. Finally, the radiation energy fluxes and the radiation powers of the Schwarzschild black hole and the Reissner--Nordstrõm black hole are derived, separately.