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     

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.     

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.     

新Tortoise坐标变换与任意加速带电动态黑洞熵

采用一种新的Tortoise坐标变换，约化视界附近Klein-Gordon方程，得到了黑洞的Hawking温度；并用薄膜模型计算了黑洞熵，得到了熵与视界面积成正比的Bekenstein关系.用这种Tortoise坐标变换，还可以使计算动态黑洞熵时所用的截断因子变得与静态和稳态情况相同. 关键词： Tortoise坐标变换 黑洞 Hawking温度 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     

新乌龟坐标变换下的动态Kinnersley黑洞的Hawking辐射

采用两种新的乌龟坐标变换,用改进的Damour-Ruffini方法研究了动态Kinnersley黑洞的Hawking辐射.在新乌龟坐标变换下,将Klein-Gordon方程在视界附近变换成平直时空的标准波动方程形式,得到了黑洞的表面引力及Hawking温度,该温度在黑洞表面不同点有不同的值.值得注意的是,旧的乌龟坐标变换存在量纲错误,新乌龟坐标变换没有量纲问题,选不同的旧乌龟坐标变换计算同一黑洞所得结果不同,但是采用不同的新乌龟坐标变换所得结果仍然不同. 关键词： 黑洞 乌龟坐标变换 Hawking辐射 Klein-Gorden方程     

Vaidya-Bonner-de Sitter时空中荷电Dirac粒子的Hawking辐射

在Vaidya-Bonner-de Siter时空中，准确地给出了黑洞内外视界及宇宙视界的位置，研究了该时空中黑洞外视界和宇宙视界附近荷电Dirac粒子的Hawking辐射，确定三个视界面中任何两个都不可能重合． 关键词：     

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     

Kerr-Newman时空中荷电Dirac粒子的Hawking辐射

本文研究任意Kerr-Newman黑洞视界曲面上荷电Dirac粒子的Hawking辐射,首先构造了一套“对称零标架”,用这套零标架计算了旋系数,导出了Dirac方程,在视界曲面附近解Dirac方程。得到荷电Dirac粒子四分量波函数的显示表式。利用解析延拓技巧,最后得到荷电Dirac粒子Hawking辐射的热谱公式。 关键词：     

一般Kerr-Newman黑洞的Dirac粒子的Hawking蒸发

本文把极端Kerr-Newman黑洞的Dirac粒子的Hawking蒸发问题推广到一般Kerr-Newman黑洞,并在黑洞的视界附近通过适当的变换找到了静止质量不为零的Dirac方程的有物理意义的解,导出了Hawking热谱公式,从而解决了Dirac粒子在一般Kerr-Newman黑洞背景下的Hawking蒸发问题。 关键词：     

Quantum Thermal Effect of Nonstatic Charged Black Hole

The difficulty of calculating energy-momentumtensors is avoided by finding directly the solution ofKlein–Gordon and Dirac equations near the horizon.Both the location of the event horizon and the Hawking radiation temperature of a nonstatic chargedblack hole are shown. The results indicate that theHawking radiation temperature can be regarded as acompensating effect under the timescaletransformation.     

Hawking thermal radiation of the dirac particle in spherically symmetric nonstatic space-time

The dynamical properties of Dirac spinor particles in a spherically symmetric nonstatic space-time are studied. The explicit representative of the four-component wave function of Dirac particles is obtained. The Dirac equation can be reduced to the standard form of the wave equation near the event horizon by the proper coordinate transformation. The event horizon location and Hawking radiation temperature are obtained.     

Hawking effect in Vaidya-Bonner space-time

A new method determining the location and the temperature of event horizons of evaporating black holes is suggested. Both the Klein-Gordon equation and the Dirac equation are studied with the method in a Vaidya-Bonner space-time. These equations are reduced near the event horizon when the generalized tortoise coordinates are adopted. The location and the temperature of the event horizon are shown automatically. The first approximation of our result is the same as that obtained by using the calculation of the vacuum expectation value of the renormalized energy-momentum tensor when the evaporation of the black hole is very slow.     

Hawking radiation from a general spherically symmetric evaporating black hole

By means of generalized tortoise coordinates both the Klein-Gordon equation and the Dirac equation are reduced near the event horizon of a general spherically symmetric evaporating black hole. The location and the temperature of the event horizon are given automatically without calculating the energy-momentum tensor. The Hawking thermal spectra of the Klein-Gordon particles and the Dirac particles are obtained, respectively.     

Einstein-Maxwell-Dilaton黑膜的狄拉克粒子辐射

分析讨论了Einstein-Maxwell-Dilaton黑膜解的视界附近的狄拉克方程.证明了在乌龟坐标变换下，该黑膜视界附近确有狄拉克粒子辐射.     

电磁直线加速动态黑洞时空中Dirac粒子的Hawking辐射

研究了作直线加速运动的电磁黑洞视界面上Dirac粒子的Hawking 辐射.首先，构造对称化零 标架，计算旋系数，导出Dirac方程，并对其进行化简.然后，通过引入广义乌龟坐标，在视 界面上将Dirac方程退耦.利用Damour-Ruffini方法，求出了温度以及热谱公式，并对所得结 果进行了讨论. 关键词： 加速动态黑洞 Dirac粒子 Dirac方程 Hawking辐射     

Stationary bound states of Dirac particles in collapsar fields

It is the first time stationary bound states of elementary spin 1/2 particles that do not decay with time are obtained for a Schwarzschild gravitational field using a self-conjugate Hamiltonian with a flat scalar product in a wide range of gravitational coupling constant. In order to obtain a discrete energy spectrum, we introduce a boundary condition such that the current density of Dirac particles near the “event horizon” is zero.     

Hawking effect in Vaidya-de Sitter space-time

The solutions of both the Klein-Gordon equation and the Dirac equation near the event horizons are given in the Vaidya-de Sitter space-time. With a new method the locations of the black hole event horizon and universe horizon, as well as their Hawking temperatures, are shown automatically and easily.