Kerr黑洞的量子面积谱及微黑洞的最小质量

Kerr黑洞仅含有两个参量M和J.把M和J视为广义坐标,并将M,J和它们的共轭量构成四维相空 间，通过规范变换得到了Kerr黑洞的量子面积谱.由此给出了Schwarzschild黑洞的 最小质量. 关键词： 黑洞 量子面积谱 共轭 规范变换     

缓变动态Kerr-Newman黑洞的量子热力学性质

引入局域热平衡概念，用Damour-Ruffini方法和薄膜模型研究了缓变动态Kerr-Newman黑洞的Hawking辐射和熵.得到了黑洞的Hawking温度和辐射谱公式，Hawking温度随时间和视界面上的位置而变化，辐射谱为准黑体谱；计算了黑洞熵，当取与静态球对称黑洞情况相同的截断关系时便得到了黑洞的Bekenstein-Hawking熵.结果表明，缓变动态黑洞的温度是局域量，缓变动态黑洞的熵与稳态黑洞情况一样正比于黑洞视界面面积. 关键词： 缓变动态黑洞 Hawking辐射 黑洞熵     

一维量子sine-Gordon模型的元激发谱

应用自洽量子微扰理论研究了由参量α₀及β₀所描述的一维量子sine-Gordon模型的元激发谱，并通过玻色化技术将所得结果与Thirring模型及半满的Hubbard模型的严格解比较．研究结果表明，导出的元激发谱描述了量子孤子及反孤子的配对激发，而自洽场给出的能隙在α₀＜1及4π≤β²₀≤8π时与严格解的结果符合较好 关键词：     

相位差与q变形广义相干叠加态的压缩特性

对于q变形的非简谐振子广义相干态的叠加态β〉+eiφβeiδ〉,其量子涨落的可能高阶压缩阶数可以表示为k≠2πn/δ,这里n是整数.当δ=π时,压缩阶数不能是偶数即只能是奇数,这正是q变形非简谐振子广义奇偶相干态的结果.由此表明参数相位差δ对决定q变形的非简谐振子广义相干态叠加态的高阶压缩阶数起决定性作用.     

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：     

从Schwarzschild黑洞到极端Kerr-Newman黑洞

考虑Schwarzschild和Kerr-Newman黑洞的度规场和电磁场张量,研究了落入黑洞的物理粒子.得出结论:任何物理粒子落入Schwarzschild或Kerr-Newman黑洞的演化过程要满足δA≥0和δκ≤0两个条件,得出了不能通过有限次操作使Kerr-Newman黑洞的温度降低到绝对零度,从而变成极端Kerr-Newman黑洞,刚好与第三定律相符.还讨论了Kerr-Newman黑洞趋于极端情况时,其面积的变化趋势,提出了黑洞负热容的影响以及熵的重整化问题. 关键词：     

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     

引力彩虹时空中Kerr黑洞的熵谱和面积谱

利用黑洞的绝热不变性,研究了引力彩虹时空中Kerr黑洞的熵谱和面积谱.首先,在引力彩虹时空背景下,计算了Kerr黑洞的绝热不变作用量,并将其与玻尔-索末菲量子化条件相结合,给出了黑洞的熵谱.得到的熵谱没有引力彩虹时空本身具有的粒子能量依赖性,且是与经典Kerr黑洞中原始贝肯斯坦熵谱相同的等间距熵谱.然后,根据黑洞热力学第一定律和黑洞熵谱,给出了与原始贝肯斯坦谱不同的面积谱.该面积谱是非等间距的,而且有对黑洞面积的依赖性,但不依赖于探测粒子的能量.面积谱表明,随着黑洞面积的减少,面积间隔逐步变小;当黑洞达到普朗克尺度时,面积量子可降为零.这表示黑洞面积不再减少,黑洞出现辐射剩余.而在忽略色散关系的修正效应或在大黑洞极限下,面积谱的修正项可以忽略,引力彩虹Kerr黑洞面积谱可以回归到原始贝肯斯坦谱.此外,对引力彩虹时空Kerr黑洞的熵进行了讨论,得到了带有面积倒数修正项的黑洞熵,分析了黑洞熵的量子修正与面积谱量子修正的一致性.     

量子体系的相空间规范变换

外尔于1918年引入的规范变换实际上是相位变换而非真正的尺度变换,但规范不变性、规范理论等概念都沿袭了下来。我们发现,针对由量子化条件[x,p]=ih而来的量子体系之本征值问题存在规范变换,或者说尺度变换,x→x/α,p→αp,该变换保体系的能量谱不变。量子谐振子、氢原子问题及一类多体问题的精确解析解证实了这一点。量子化条件[x,p]=ih看来是个对量子力学很强的约束,不止于能量的量子化。这个规范变换提醒我们相空间的体积及其量子化才是物理的关键,这也是量子力学和统计物理在潜意识里一直沿用却未予关注的思路。有趣的是,从量子谐振子体系的相空间表述似乎不能导向这个结论。如同规范理论所断言的电磁学量在给定坐标系下的数值表征与标度无关,我们认为量子体系的物理量,如能量谱等,在给定坐标系下的数值表征亦应与标度无关。此尺度变换与德布罗意关系相恰。     

非简谐振子的奇偶广义相干态

把奇偶相干态推广到了非简谐振子的势场中，发现随着平均能量的增加，奇偶广义相干态交替出现压缩现象．在随时间的演化过程中，自然坐标与自然动量的量子起伏产生周期为π／２的压缩 关键词：     

Thermodynamics Properties of the Inner Horizon of?a?Kerr-Newman Black Hole

In this paper, we study the thermal properties of the inner horizon of a Kerr-Newman black hole. By adopting Damour-Ruffini method and the thin film model which is developed on the base of brick wall model suggested by ’t Hooft, we calculate the temperature and the entropy of the inner horizon of a Kerr-Newman black hole. We conclude that the temperature of inner horizon is positive and the entropy of the inner horizon is proportional to the area of the inner horizon. The cut-off factor is same as it in calculation of the entropy of the outer horizon, 90β. In addition, we write the integral and differential Bekenstein-Smarr formula as the parameters of the inner horizon. Then, we discuss that if the contribution of the inner horizon is taken into account to the total entropy of the black hole, the Nernst theorem can be satisfied. At last, We calculate the tunneling rate of the outer horizon Γ₊ and the inner horizon Γ₋. The total tunneling rate Γ should be the product of the rates of the outer and inner horizon, Γ=Γ₊⋅Γ₋. We find that the total tunneling rate is in agreement with the Parikh’s standard result, Γ→exp (ΔS _BH ), and there is no information loss.     

Kerr-Newman黑洞的熵修正

基于Majhi等人最近的工作,利用狄拉克方程,在半经典近似外讨论了Kerr-Newman黑洞的熵修正.在单位制G=c=kB=1下,由于普朗克常数与普朗克长度,普朗克质量和普朗克电荷的平方成正比,作用量的量子修正项与半经典项的比例常数被选为(Mrh-Q2/2)-1.结合视界方程的微分形式和黑洞热力学第一定律,本文得到了荷电稳态黑洞的修正熵并发现修正项同样包括Bekenstein-Hawking熵的对数项和倒数项.     

量子史瓦茨黑洞和暗物质

引入Sommerfeld作用量量子化条件来处理Schwarzschild黑洞的量子化问题. 发现此类量子化黑洞存在一个质量为m_G=123m_p的基态，处于基态的量子Schwarzschild黑洞不再存在Hawking蒸发和任何其他辐射，可名之曰暗星. 它的存在不仅可以解决信息丢失的疑难，而且极可能是构成暗物质的主要候选者. 关键词： 量子史瓦茨黑洞 暗物质     

Gedanken experiments to destroy a black hole

It is widely believed that the complete gravitational collapse of a body always results in a black hole (i.e., “naked singularities” can never be produced) and that all black holes eventually “settled down” to Kerr-Newman solutions. An important feature of the Kerr-Newman black holes is that they satisfy relation m² ? a² + e² where m is the mass of the black hole, e is its charge, $\text{a =}\text{J}\text{m}$ is its angular momentum per unit mass and geometrized units G = c = 1 are used. (For m² <a² + e² the Kerr-Newman solutions describe naked singularities.) In this paper, we test the validity of the above conjectures on gravitational collapse by attempting to create a spacetime with m² <a² + e² starting with a Kerr-Newman black hole with m² = a² + e². Such a spacetime would either have to be a new black hole solution or a “naked singularity,” in violation of the above conjectures. In the first gedanken experiment we attempt to make the black hole capture a test particle having large charge and orbital angular momentum compared with energy. In the second gedanken experiment we attempt to drop into the black hole a spinning test body having large spin to mass ratio. In both cases we find that bodies which would cause violation of m² ? a² + e² will not be captured by the black hole, and, thus, we cannot obtain m² <a² + e², although we can come arbitrarily close in the sense that m² = a² + e² can be maintained in these processes.     

Quantization of Kerr-Newman Black Hole Entropy

Kerr-Newman black hole entropy in phase space is systematically investigated by constructing the six-dimensional phase space within gauge transformation. Then considering the corresponding mechanical quantities as operators and making them quantized, entropy spectrum of Kerr-Newman black hole is obtained. Our results demonstrate that Kerr-Newman black hole has an equal-interval entropy spectrum, which coincides with the view of Bekenstein. It also shows that Kerr-Newman black hole entropy is not zero, but exists a ground-state entropy, which still retains some basic information.     

Effective Values of Komar Conserved Quantities and Their Applications

We calculate the effective Komar angular momentum for the Kerr-Newman (KN) black hole. This result is valid at any radial distance on and outside the black hole event horizon. The effective values of mass and angular momentum are then used to derive an identity (K_c^m=2STK_{\chi^{\mu}}=2ST) which relates the Komar conserved charge (K_c^mK_{\chi^{\mu}}) corresponding to the null Killing vector (χ ^μ ) with the thermodynamic quantities of this black hole. As an application of this identity the generalised Smarr formula for this black hole is derived. This establishes the fact that the above identity is a local form of the inherently non-local generalised Smarr formula.     

Charged Fermions Tunnel from the Kerr-Newman Black Hole Influenced by Quantum Gravity Effects

Taking into account quantum gravity effects, we investigate the tunnelling radiation of charged fermions in the Kerr-Newman black hole. The result shows that the corrected Hawking temperature is determined not only by the parameters of the black hole, but also by the energy, angular momentum and mass of the emitted fermion. Meanwhile, an interesting found is that the temperature is affected by the angle ??. The quantum gravity correction slows down the evaporation.     

Cosmic string in the NUT-Kerr-Newman spacetime

We study the equilibrium configurations of a cosmic string described by the Nambu action in the NUT-Kerr-Newman spacetime which includes as special cases the Kerr-Newman black hole spacetime as well as the NUT spacetime which is considered as a cosmological model. In this study it is interesting to note that one can obtain parallel results for the Kerr-Newman black hole as well as the NUT spacetime.     

Black Hole Complementary Principle and Noncommutative Membrane

In the spirit of black hole complementary principle, we have found the noncommutative membrane of Scharzchild black holes. In this paper we extend our results to Kerr black hole and see the same story. Also we make a conjecture that spacetimes are noncommutative on the stretched membrane of the more general Kerr-Newman black hole.