Kerr-Newman黑洞的谐振子模型及量子面积谱

利用Kerr-Newman黑洞的质量M,电量Q,角动量J和它们各自的对偶量,π_M,π_Q,π_J,构成的六维相空间,通过规范变换,首先建立黑洞的简谐振子模型;再利用该模型进一步研究Kerr-Newman黑洞的量子面积谱.关键词：黑洞规范变换简谐振子模型量子面积谱     

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.     

黑洞量子理论

简述引力场中物质的量子效应——黑洞的Ｈａｗｋｉｎｇ辐射，并进一步讨论黑洞的量子理论，给出一些结论。     

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．     

经典Kerr黑洞和量子Kerr黑洞系统的微正则系综理论描述与统计“自举”条件

分别从Kerr黑洞的经典谱和量子谱出发,建立了一个居于微正则系综理论描述的系统态密度 的不等式,并由此证明了Kerr黑洞满足统计“自举(bootstrap)”条件.其主要结论是对于由 大量Kerr黑洞组成的体系,在高能极限下,最可能的构型是一个黑洞将获得系统所有的质量 和全部的角动量,而且转动不会破坏黑洞的“自举”性质.关键词：Kerr黑洞统计“自举”问题     

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     

变加速直线运动黑洞的量子热效应

给出了作变加速直线运动的蒸发黑洞的辐射温度。此温度不仅随时间变化,而且在视界的同时面上不是常数。这种黑洞的视界位置随时间变化,而且形状不是球对称的。关键词：     

Kerr效应对二项式腔场谱量子干涉的影响

研究了含Kerr介质高Q腔内单个二能级原子与双模二项式光场发生双光子共振相互作用系统的腔场谱,给出了Kerr效应与量子干涉项ΔS(ω)关系的数值计算结果,讨论了Kerr效应对二项式腔场谱量子干涉的影响.结果表明:若初始时刻原子处于激发态而双模光场处于二项式态,随Kerr效应的增强,致使量子干涉项引起谱线强度的改变量呈现出\"不规则的周期性衰减振荡\"特性,震荡幅度与两模光场的频差密切相关.在Kerr系数χg(g为光场与原子的耦合常数)时,Kerr效应对干涉项的影响比较强烈;在χg时,趋于平稳.随着Kerr效应的增强,系统腔场谱由对称结构逐渐演化为不对称的多谱线结构.     

Kerr 时空黑洞熵和测不准关系

通过应用在量子引力中、由广义测不准关系得出的新的态密度方程,直接求解轴对称Kerr黑洞背景下Bose场和Fermi场的配分函数.然后,在黑洞视界附近计算黑洞背景下Bose场和Fermi场的熵.在所得结论中不存在用brick wall模型计算黑洞熵时出现的发散项,也不存在紫外因子.得到黑洞熵与视界面积成正比的结论.     

自旋场对Barriola-vilenkin黑洞熵的量子修正

用砖墙模型的方法,讨论了无源引力场对Barriola-Vilenkin黑洞熵的量子修正.计算表明, 量子修正应该包含两部分：其中一部分与视界面积成正比,在视界附近与紫外截断因子是 平方反比发散的;另一部分是两个对数发散项,这部分除了与黑洞的本身特征性质(M,η) 有关以外,还与自旋场的自旋有关.结果与标量场引起的量子修正具有完全不同的形式.关键词：砖墙模型量子修正黑洞熵     

Universal canonical entropy for gravitating systems

The thermodynamics of general relativistic systems with boundary, obeying a Hamiltonian constraint in the bulk, is determined solely by the boundary quantum dynamics, and hence by the area spectrum. Assuming, for large area of the boundary, (a) an area spectrum as determined by non-perturbative canonical quantum general relativity (NCQGR), (b) an energy spectrum that bears a power law relation to the area spectrum, (c) an area law for the leading order microcanonical entropy, leading thermal fluctuation corrections to the canonical entropy are shown to be logarithmic in area with a universal coefficient. Since the microcanonical entropy also has universal logarithmic corrections to the area law (from quantum space-time fluctuations, as found earlier) the canonical entropy then has a universal form including logarithmic corrections to the area law. This form is shown to be independent of the index appearing in assumption (b). The index, however, is crucial in ascertaining the domain of validity of our approach based on thermal equilibrium.     

Canonical Entropy of Reissner-Nordstrom Black Hole

Recently, Hawking radiation of the black hole has been studied using the tunnel effect method. It is found the radiation spectrum of the black hole is not a strictly pure thermal spectrum. How the departure from pure thermal spectrum affects the entropy? This is a very interesting problem. In this paper, we calculate the partition function by energy spectrum obtained by tunnel effect. Using the relation between the partition function and entropy, we derive the expression of entropy the general charged black hole. In our calculation, we not only consider the correction to the black hole entropy due to fluctuation of energy but also consider the effect of the change of the black hole charges on entropy. We discuss Reissner-Nordstrom black hole and obtain that Reissner-Nordstrom black hole cannot approach the extreme black hole by changing its charges.     

正则黑洞熵与相变

应用隧道效应对黑洞Hawking辐射研究得到的辐射谱,对非旋转黑洞的正则熵进行讨论.所得熵遵守Bekenstein-Hawking 面积定律,并带有修正项,主要修正项与面积的对数成正比,另有与黑洞热容量有关的修正项.利用所给出的正则熵,对黑洞的相变进行讨论,得到当黑洞的热容量出现发散时,正则熵在该处并不出现复数,由此认为此相变为二级相变.关键词：正则系综量子修正黑洞相变     

Interacting Bosons at Finite Temperature: How Bogolubov Visited a Black Hole and Came Home Again

The structure of the thermal equilibrium state of a weakly interacting Bose gas is of current interest. We calculate the density matrix of that state in two ways. The most effective method, in terms of yielding a simple, explicit answer, is to construct a generating function within the traditional framework of quantum statistical mechanics. The alternative method, arguably more interesting, is to construct the thermal state as a vector state in an artificial system with twice as many degrees of freedom. It is well known that this construction has an actual physical realization in the quantum thermodynamics of black holes, where the added degrees of freedom correspond to the second sheet of the Kruskal manifold and the thermal vector state is a state of the Unruh or the Hartle–Hawking type. What is unusual about the present work is that the Bogolubov transformation used to construct the thermal state combines in a rather symmetrical way with Bogolubov's original transformation of the same form, used to implement the interaction of the nonideal gas in linear approximation. In addition to providing a density matrix, the method makes it possible to calculate efficiently certain expectation values directly in terms of the thermal vector state of the doubled system.     

Area spectrum of the three-dimensional Godel black hole

<正>The aim of this paper is to investigate the area spectrum of the three-dimensional Godel black hole by using two different methods.The result shows that the area spectrum of the black hole is△A = 8πl_p~2,which confirms the initial proposal of Bekenstein that the area spectrum is independent of black hole parameters and the spacing is 8πl_p~2.