能斯特定理与黑洞的普朗克绝对熵

考虑Kerr黑洞内视界处的热性质后,给出了Bekenstein-Smarr公式的新形式,重新定义了黑洞熵.黑洞温度趋于绝对零度时,新定义的黑洞熵一定趋于零.它满足能斯特定理,可视为黑洞的普朗克绝对熵. 关键词：     

黑洞的视界面公式

从零曲面方程出发,导出了黑洞视界面的普遍公式.利用高登方程验证了该公式的正确性,并利用该公式求出了任意加速含荷黑洞的视界. 关键词： 黑洞 视界 零曲面 乌龟坐标变换     

球对称带电蒸发黑洞的视界与温度

本文从讨论视界附近的Klein-Gordon方程出发,直接准确地算出球对称带电蒸发黑洞事件视界的位置和考虑反作用后的Hawking辐射温度,而无需求助于低维能-动张量的近似计算。 关键词：     

黑洞碰撞的模拟

当加速黑洞的视界与其Rindler视界接触的时候,黑洞变形为椭球状,接触点的HawkingUnruh温度降低到绝对零度,而黑洞尾部的温度趋于无穷大,形成高温喷流.此结果可以看作两个黑洞碰撞的模拟.预期黑洞碰撞时接触点的温度会降低到绝对零度,而两个黑洞尾部的温度均会趋于无穷大,出现反向的高温喷流 关键词：     

Kerr-NUT黑洞的表面几何

本文给出了Kerr-NUT黑洞视界高斯曲率的解析表达式,分析了NUT参数对视界的赤道周长和极向周长的影响,研究了将其视界嵌入欧几里得空间的问题。结果表明这种黑洞的视界具有其它黑洞所没有的几何性质。 关键词：     

关于普朗克公式的一点讨论

对普朗克公式中谐振子的物理意义进行了讨论,认为普朗克在推导其黑体辐射公式时所使用的谐振子模型实际上就是腔内的电磁波模式。     

两个Schwarzschild黑洞的表面几何

计算了两个Schwarzschild黑洞视界的高斯曲率、赤道周长和极向周长。研究了这些量随两个黑洞之间的距离不同而产生的变化。结果表明两个黑洞中的一个对另一个视界几何性质的影响。 关键词：     

一般球对称带电蒸发黑洞的温度

从视界附近的KleinGordon方程出发,准确地定出了一般球对称带电蒸发黑洞的Hawking温度和辐射谱,同时计算出事件视界方程.所得结果与用零曲面方程得到的结果一致 关键词： 蒸发黑洞 视界 辐射     

认识黑洞的首个直接“视觉”证据

2019年4月10日,由黑洞事件视界望远镜（Event Horizon Telescope,EHT）合作组织协调召开新闻发布会,全球多地同时发布了黑洞的首个直接“视觉”证据。作为人类捕获的首张黑洞照片,它展示了5500万光年外的椭圆星系M87中心超大质量黑洞的图像,看到了黑洞“阴影”和周围环绕的新月状光环。EHT的此次观测结果从强引力场的角度验证了爱因斯坦广义相对论,有助于研究黑洞的吸积以及喷流的产生。文章着重介绍为什么给黑洞“拍照”,选择哪些黑洞模特“拍照”,如何给黑洞“拍照”,获得的数据经过怎样的后期处理和分析才能生成大家看到的“照片”;此外还将介绍在此次合作项目里的中国贡献,最后对黑洞高分辨率成像领域进行展望。     

黑洞温度的奇异特性—量子温度

从经典理论看来，黑洞温度只能是绝对零度．只有考虑了黑洞的量子效应之后，黑洞才具有以视界引力加速度所标志的确定温度值．本文讨论了黑洞温度的这一奇异特性．     

Kim黑洞熵与能斯特定理

从Kim时空背景下的Klein-Gordon方程出发,利用brick-wall方法计算标量场的自由能和熵.得到标量场的熵不仅与黑洞的外视界面积有关,而且也是内视界面积的函数.所得结论,当取某种近似时,可得到熵只与外视界面积成正比的关系.并且表明,用内外视界位置参量表达的熵,在黑洞辐射温度趋于绝对零度时,黑洞的熵也趋于零,它满足能斯特定理,可视为黑洞的普朗克绝对熵 关键词： brick-wall方法 黑洞熵 能斯特定理     

THE ELECTRON IN THE GRAVITATIONAL FIELD OF THE KERR BLACK HOLE

We investigate the electronic energy levels in the field of the micro-Kerr black hole under the approximation condition a<2, and obtain some interesting results.     

满足热力学第三定律的修正的黑洞的熵公式

认为黑洞的熵正比于视界面积的熵公式S=A/4不能满足热力学第三定律,提出了新的熵公式,它既能满足热力学第三定律,又能推出黑洞的温度的表达式. 关键词： 黑洞 熵 热力学第三定律     

THERMODYNAMICS OF THE SLOWLY ROTATING KERR-NEWMAN BLACK HOLE IN THE GRAND CANONICAL ENSEMBLE

We investigate the thermodynamics of the slowly rotating Kerr-Newman (K-N) black hole in the grand canonical ensemble with York's formalism. Some thermodynamical properties, such as the thermodynamical action, entropy, thermodynamical energy and heat capacity are studied, and solutions of the slowly rotating K-N black hole with different boundary conditions are analysed. We find stable solutions and instantons under certain boundary conditions.     

MASSIVE SCALAR PARTICLE IN THE GRAVITATIONAL FIELD OF A MICROCOSMIC BLACK HOLE

The finite motion of a massive scalar particle in the gravitational field of a microcosmic black hole with weak relativistic approximation is discussed. In the Schwarzschild field, using the condition for balance σ=0, we obtain the relation between the produced and captured amplitudes for particles. In the Kerr field we show that the attenuation depends on the moment of the black hole and the attenuation process becomes an exciting one when ωh.     

QUASILOCAL ENERGY FOR STATIONARY AXISYMMETRIC EMDA BLACK HOLE

By using Brown-York quasilocal energy theory we calculate the quasilocal energy of a stationary axisymmetic EMDA black hole and explore the universality of Martinez's conjecture in string theory. We show that the energy is positive and monotonically decreases to the ADM mass at spatial infinity, and the Martinez's conjecture, the Brown-York quasilocal energy at the outer horizon reduces to twice its irreducible mass, is still valid for stationary axisymmetric EMDA black hole. From the result we also find that the Kerr-Sen spacetime keeps up with Martinez's conjecture. This is different from the Bose-Naing result that the quasilocal energy of the Kerr-Sen spacetime does not approach the Martinez's conjecture.     

Violation of the second law of black hole physics by tachyons

It is shown that the interaction of a class of positive energy tachyons decreases the area of the horizon of theT-S, ∂=3 metric even in the case of a reversible transformation (M _ir=constant). This is a violation of the second law of black hole physics.     

NON-THERMAL RADIATION FROM A NON-KERR－NEWMAN BLACK HOLE

In the spacetime of a charged spinning black hole, the distribution of particle energy levels has been studied. Near the event horizon of such a black hole a crossing of the particle energy levels exists, which leads to the occurrence of non-thermal radiation of the black hole. This quantum effect is non-thermal and also different from those of the Kerr and Kerr－Newman black holes.