Kerr介质中压缩真空场与耦合双原子依赖强度耦合系统原子布居数的时间演化

研究了存在Kerr介质时,单模压缩真空场与耦合双原子依赖强度耦合相互作用系统原子布居数的时间演化规律,讨论了Kerr介质、原子间相互作用和光场的初始压缩因子对原子布居数时间演化的影响.     

耦合双原子与压缩真空场Raman相互作用的动力学

研究了耦合双原子与单模压缩真空场Raman相互作用过程中原子布居和偶极压缩的时间演化特性,运用数值方法讨论了系统耦合常数和初始状态对原子动力学行为的影响 关键词： 耦合双原子 压缩真空场 Raman相互作用 原子布居 原子偶极压缩     

被克尔介质包围的A型三能级原子的粒子布居几率

本文研究了被克尔(Kerr)介质包围的\型三能级原子的粒子布居几率随时间的演化,分析了光场频率与原子本征频率间的单光子失谐量和克尔介质对粒子布居几率的影响.     

Kerr介质中双光子T-C模型光场的量子特性

研究了存在Kerr介质时，耦合双原子与单模压缩真空场双光子跃迁相互作用系统光场的量子特性，讨论了Kerr介质和原子间偶极-偶极相互作用对光场量子特性的影响. 结果表明：当Kerr效应和偶极-偶极相互作用可以忽略时，光场U2分量的涨落能被周期性地压缩，随着Kerr效应和偶极-偶极相互作用的增强，光场的压缩逐渐变浅，压缩次数减少；Kerr效应和偶极-偶极相互作用的影响使光场的二阶相干度时间演化曲线呈现周期性的崩塌-回复现象，但不论耦合强度如何，光子总是呈现聚束效应. 关键词： Kerr介质 压缩真空场 耦合双原子 光场的量子特性     

Kerr介质中耦合双原子与双模压缩真空场相互作用系统的光子统计性质

研究了存在Kerr介质时，双模压缩真空场与耦合二能级原子相互作用系统中光子的统计性质，讨论了Kerr介质与光场的耦合强度、光场的初始压缩因子和原子的初态对光子统计性质的影响.数值计算结果表明，光子周期性地交替呈现聚束和反聚束效应，光场两模之间总是呈现正相关，并且这种相关为非经典相关；Kerr介质的影响使光场的二阶相干度演化曲线呈现周期性的崩塌-回复现象，随着Kerr效应的加强，崩塌-回复周期变短，以至消失. 关键词： Kerr介质 耦合双原子 双模压缩真空场 光子统计性质     

Kerr介质中双模SU(1,1)相干态场与V型三能级原子的相互作用

导出了充满Kerr介质的高Q腔中V型三能级原子与双模SU（1，1）相干态场相互作用系统的态矢量，并以此计算三能级原子布居概率和辐射场统计性质随时间的演化．数值计算显示，Ker效应产生与两能级原子不同的Rabi振荡特性，而双模场的关联特性受Kerr介质的影响较小．还讨论了Ker效应对Cauchy-Schwartz不等式的影响． 关键词：     

附加Kerr介质依赖强度耦合负二项式光场与二能级原子的相互作用

采用数值计算的方法,研究了有Kerr介质存在时负二项式光场与二能级原子依赖强度耦合相互作用系统中原子布居反转的时间演化规律,讨论了Kerr介质和光场参量对原子反转的时间演化的影响.     

Kerr介质中非关联双模相干态光场与V型三能级原子的相互作用

导出了充满Kerr介质的高Q腔中非关联双模相干态光场与V型三能级原子相互作用系统的态矢量, 通过数值计算,分析了光与原子之间单光子失谐量和Kerr介质对原子能级布居概率及光的量子统计特性的影响,给出了原子布居概率和双模场量子统计特性的时间演化曲线.结果表明, 原子布居概率受Kerr效应的影响较大,且在该曲线上附加一低频起伏. 通过对双模光场二阶相干度的分析:一模呈现亚泊松分布;另一模呈现超泊松分布.     

两纠缠原子与二项式光场相互作用的动力学

采用时间演化算符和数值计算方法，研究了两全同二能级纠缠原子与二项式光场相互作用的动力学，结果表明原子布居和原子偶极压缩的时间演化与二项式光场系数和两纠缠原子的纠缠度有很强的关联，选择合适的系统参数，原子偶极矩可以被完全压缩. 关键词： 纠缠原子 二项式态 原子布居 偶极压缩     

高Q Kerr介质腔中SU(2)相干态光场与Λ型三能级原子的相互作用

研究了一位于高 Q Kerr介质腔中的 SU(2 )相干态光场与 Λ型三能级原子相互作用系统中 ,Kerr效应对三能原子布居概率、光子统计分布、光场的模间相关性、Cauchy- Schwartz不等式以及光场差压缩的影响 .结果表明 ,较强的 Kerr效应可使原子 Rabi振荡呈现明显的崩溃与回复现象 ,而使场的非经典相关程度减弱 ,但适当强度的 Kerr效应可使光场差压缩程度明显增强 .     

Causality violation in the Kerr metric

The conjecture that geodesics in the Kerr matric witha > m cannot violate causality in the sense of meeting a turning point before making up for lost time, is found to be untrue for null geodesics.     

Kerr metric in the deSitter background

In addition to the Kerr metric with cosmological constant Λ several other metrics are presented giving a Kerr-like solution of Einstein’s equations in the background of deSitter universe. A new metric of what may be termed as rotating deSitter space-time—a space-time devoid of matter but containing null fluid with twisting null rays, has been presented. This metric reduces to the standard deSitter metric when the twist in the rays vanishes. Kerr metric in this background is the immediate generalization of Schwarzschild’s exterior metric with cosmological constant.     

Stationary frames in the Kerr field

Stationary frames in the Kerr geometry are rewieved and their properties compared. In particular, the locally non-rotating frame, the Carter frame, the static frame and the frame connected with the equatorial circular geodesic are treated as the most important examples.     

Polar orbits in the Kerr space-time

The motion of test particles in polar orbit about the source of the Kerr field of gravity is studied, using Carter's first integrals for timelike geodesies in the Kerr space-time. Expressions giving the angular coordinates of such particles as functions of the radial one are derived, both for the case of a rotating black hole as well as for that of a naked singularity.     

Boosting the Kerr metric

An exact solution of Einstein's equations describing the gravitational wave associated to a ring of massless particles is presented. It has been obtained by boosting the Kerr metric along the axis of symmetry, and considering the limit in which the speed of the boost tends to the velocity of light.     

Race for the Kerr field

Roy P. Kerr has discovered his celebrated metric 45 years ago, yet the problem to find a generalization of the Schwarzschild metric for a rotating mass was faced much earlier. Lense and Thirring, Bach, Andress, Akeley, Lewis, van Stockum and others have tried to solve it or to find an approximative solution at least. In particular Achilles Papapetrou, from 1952 to 1961 in Berlin, was interested in an exact solution. He directed the author in the late autumn of 1959 to work on the problem. Why did these pre-Kerr attempts fail? Comments based on personal reminiscences and old notes.     

Imaginary Weyl coordinates in the Kerr space-time

By introducing imaginary Weyl coordinates the Kerr geometry can be described by the Weyl coordinate system as good as the Boyer-Lindquist system.     

Parametrization of the Kerr Solution

From the Kerr solution of Ernst equation under Ehlers and unitary transformations, we build a parametrized Kerr solution depending on three parameters, namely the mass, the angular momentum of the source and an adimensional parameter m ₁. Varying m ₁ produces a topological deformation of the ergosphere.     

Characterizations of the Kerr metric

For stationary, asymptotically flat solutions of Einstein's equations, covariant functionals of the metric variables are defined which characterize the Kerr metric uniquely. For instance, we obtain a generalization of the Bach tensor to stationary metrics, which vanishes if and only if the solution is Kerr. We also give a new interpretation of the Schwarzschild-to-Kerr-transformation. Our results might be applicable to simplify the proof of the uniqueness theorem for stationary black holes.