自旋-轨道耦合作用下双组分量子气体中的动力学结构因子与求和规则

在自旋-轨道耦合作用下,双组分量子气体中密度涨落和自旋涨落的动力学结构因子满足不同形式的求和规则.特别是动力学结构因子的一阶矩一般不具有空间反演对称性.针对两个特定的模型——Raman耦合作用下的无相互作用费米气体与弱相互作用玻色气体,分别计算了在不同参数条件下密度涨落和自旋涨落的动力学结构因子,并讨论了实验上观测其一阶矩偏离空间反演对称所需达到的能谱分辨率.     

一种推导二能级原子自发辐射方法

考虑真空涨落能量为负的特点,提出一个能够简洁描述原子与真空涨落相互作用的方程,得到原子处于激发态的概率随时间变化的关系,讨论了原子自发辐射的速率与真空涨落的强度的关系.     

具有随机色散的光时分复用系统中色散管理孤子相互作用

本文采用变分法和数值方法研究了具有随机色散的光时分复用系统中色散管理孤子相互作用.发现随机色散增强了孤子间相互作用, 产生了导致孤子淹没的振幅和间隔涨落.相互作用距离与初始间隔、初始相对相位、脉宽和初始相对振幅有关.     

V型三能级原子与非经典光场作用中光场特性的变化

研究了V型三能级原子BEC与双模压缩光场相互作用系统中,忽略原子间相互作用和考虑原子间相互作用时光场的正交压缩和光子数压缩。结果表明,光场的正交压缩依赖于压缩参数,而光子数压缩与压缩参数、光场信号强度有关,在一定条件下,两种压缩可同时存在。原子间相互作用影响两种压缩的涨落随时间变化的周期,以及正交分量涨落随时间变化的幅度,而对光子数压缩涨落随时间变化的幅度几乎无影响。     

相互作用原子玻色-爱因斯坦凝聚体诱导的光场压缩效应

给出了光场与二能级原子玻色-爱因斯坦凝聚体(BEC)相互作用系统的哈密顿量，研究了原子 间相互作用对压缩相干态光场与原子BEC相互作用系统中光场正交压缩特性的影响.结果表明 ：光场两正交分量的涨落均随时间按余弦规律周期性地变化，其压缩性质依赖于光场的初始 压缩因子和压缩方向角，而原子间的相互作用影响光场正交分量的涨落随时间变化的幅度和 周期. 关键词： 玻色-爱因斯坦凝聚 压缩相干态 光场的正交压缩     

在与原子相互作用中光偏振态的量子描述及其演化

应用偏振光的量子理论和斯托克斯算符研究了无克尔媒质和存在克尔媒质情况下，光在与原子相互作用过程中偏振态的演化.研究了偏振光中斯托克斯参量的涨落及其压缩的非经典行为.偏振椭圆、量子光学中的偏振度和斯托克斯参量的信噪比也得到了讨论.结果表明斯托克斯参量及其涨落在时间演化中呈现出被调制的振荡，这些振荡表现出间歇地崩塌和恢复.在与原子的相互作用过程中，光的偏振椭圆不随时间变化，但偏振度却随时间出现振荡.克尔媒质对这些振荡演化有很大影响. 关键词： 斯托克斯算符 斯托克斯参量 量子偏振态 量子涨落     

双色驻波场中梯形三能级原子所受整流偶极力的涨落分析

本文基于文献[1]利用双色驻波场作用于三能级原子获得宏观数量个光学波长上符号保持不变的整流偶极力的工作基础上,运用量子回归定理计算了所得整流偶极力在一个光学波长上的涨落.结果表明:原子偶极零点振动与光场幅度梯度相互作用引起的偶极力的涨落D1的值较大,是整流偶极力涨落的主要因素,且其随空间的变化规律与整流偶极力相似;原子偶极与真空零点振动相互作用导致偶极力的涨落Ds较小,几乎可以忽略不计.由于力的起伏所导致的加热效应不利于中性原子的偶极束缚[6].     

受激拉曼增益介质中的量子噪声特性研究

研究了三能级原子系综与相干控制场以及量子探测场的相互作用下的受激拉曼系统.运用量子理论推导出了该受激拉曼系统中由于量子场真空涨落引起的量子噪声以及受激散射的量子化光场噪声谱,并且数值计算了注入拥有非经典涨落的量子探测场,真空涨落所引起的量子噪声谱. 关键词： 受激拉曼增益 量子噪声 噪声谱     

Coherent Resonance for Rate Oscillations During CO Oxidation on Pt(110) Surfaces: Interplay Between Internal and External Noise

用理论和模拟相结合的方法研究了Pt(110)面上CO催化氧化体系中由化学反应随机性所导致的内涨落和参量扰动带来的外涨落对其速率振荡过程的影响,重点考察了内涨落和外涨落的相互作用．在体系的确定性Hopf分岔点附近区域,噪声可以诱导产生随机振荡,其信噪比随噪声强度的变化会出现极大值,即发生了相干共振．运用随机范式理论,研究发现体系的相干共振行为依赖于一\有效噪声",其强度是内涨落和外涨落的加权和．研究结果表明,在内外噪声强度的参数平面内,随机振荡的信噪比呈现屋脊形,太大的内涨落或外涨落条件下相干共振都不能发生．数值模拟的结果和理论分析符合得很好．     

压缩真空场与耦合双原子Raman相互作用过程中光场的相位演化特性

采用Pegg-Barnett相位理论，研究了压缩真空场与耦合双原子Raman相互作用过程中光场的相位演化特性.具体计算了场的相位概率分布函数及相位涨落，给出了在极坐标中概率分布变化曲线.讨论了原子与场相互作用、两原子间偶极-偶极相互作用以及原子初始状态对光场相位性质的影响. 关键词： 相位特性 压缩真空场 耦合双原子 Raman相互作用     

Agegraphic Dark Energy with the Sign-Changeable Interaction in Non-Flat Universe

In this paper,we investigate the agegraphic dark energy(ADE) model by including the sign-changeable interaction between ADE and dark matter in non-flat universe.The interaction Q can change its sign from Q 0 to Q 0 as the universe expands.This indicates that at first dark matter decays to ADE,and then ADE decays to dark matter.We study the dynamical behavior of the model by using the phase-plane analysis.It is shown numerically that the coupling constant β plays an important role in the evolution of the universe.The equation of state(Eo S) of ADE with the sign-changeable interaction is more likely to cross the phantom divide w_d =-1 from top to bottom with the increasing of the |β|.Whereas in ADE model with usual interaction,wd can cross the phantom divide from bottom to top.We also find that our model is consistent with the observational data.     

Generalized Ghost Pilgrim Scalar Field Models of Dark Energy

We assume generalized ghost Pilgrim dark energy (GGPDE) model in the presence of cold dark matter in flat FRW universe. With suitable choice of interaction term between GGPDE and cold dark matter, we investigate the nature of equation of state parameter for GGPDE. Also, we investigate the natures of dynamical scalar field models (such as quintessence, tachyon, k-essence, and dilaton dark energy) and concerned potentials through the correspondence phenomenon between GGPDE and these models.     

Entropy-Corrected Holographic Dark Energy

The holographic dark energy (HDE) is now an interesting candidate of dark energy, which has been studied extensively in the literature. In the derivation of HDE, the black hole entropy plays an important role. In fact, the entropy-area relation can be modified due to loop quantum gravity or other reasons. With the modified entropy-area relation, we propose the so-called ``entropy-corrected holographic dark energy' (ECHDE) in the present work. We consider many aspects of ECHDE and find some interesting results. In addition, we briefly consider the so-called ``entropy-corrected agegraphic dark energy' (ECADE).     

New Agegraphic Dark Energy in Brans-Dicke Theory

In this paper, we investigate the new agegraphic dark energy model in the framework of Brans-Dicke theory, which is a natural extension of the Einstein's general relativity. In this framework the form of the new agegraphic dark energy density takes as ρ_q =3n² φ(t) η^-2, where η is the conformalage of the universe and φ(t) is the Brans-Dicke scalar field representing the inverse of the time-variable Newton's constant. We derive the equation of state of the new agegraphic dark energy and the deceleration parameter of the universe in the Brans-Dicke theory. It is very interesting to find that in the Brans-Dicke theory the agegraphic dark energy realizes quintom-like behavior,i.e., its equation of state crosses the phantom divide w=-1 duringthe evolution. We also compare the situation of the agegraphic darkenergy model in the Brans-Dicke theory with that in the Einstein'stheory. In addition, we discuss the new agegraphic dark energy modelwith interaction in the framework of the Brans-Dicke theory.     

暗孤子的周期性再生效应

通过数值求解变系数非线性薛定谔方程,讨论具有有限背景宽度的皮秒暗光脉冲的传输和相互作用。结果表明,一种新的效应,即暗孤子的周期性再生效应,稳定地存在于具有分布参量的光纤系统中,不会受到孤子间相互作用的影响。并且,这种再生效应对损耗和有限的扰动(如白噪声)等不敏感。这表明暗孤子的周期性再生效应是稳定的。     

Holographic Gas as Dark Energy

We investigate the statistical nature of holographic gas, which may represent the quasi-particle excitations of a strongly correlated gravitational system. We find that the holographic entropy can be obtained by modifying degeneracy. We calculate thermodynamical quantities and investigate stability of the holographic gas. When applying to cosmology, we find that the holographic gas behaves as holographic dark energy, and the parameter c in holographic dark energy can be calculated from our model. Our model of holographic gas generally predicts c 〈 1, implying that the fate of our universe is phantom-like.     

Modified Holographic Ricci Dark Energy in Chameleon Brans–Dicke Cosmology and Its Thermodynamic Consequence

The objective of this paper is to discuss the Chameleon Brans–Dicke gravity with non-minimally matter coupling of scalar field. We take modified Holographic Ricci dark energy model in this gravity with its energy density in interaction with energy density of cold dark matter. We assume power-law ansatz for scale factor and scalar field to discuss potential as well as coupling functions in the evolving universe. These reconstructed functions are plotted versus scalar field and time for different values of power component of scale factor n. We observe that potential and coupling functions represent increasing behavior, in particular, consistent results for a specific value of n. Finally, we have examined validity of the generalized second law of thermodynamics and we have observed its validity for all values of n.     

Dark energy interacting with dark matter and a third fluid: Possible EoS for this component

A cosmological model of dark energy interacting with dark matter and another general component of the universe is considered. The equations for the coincidence parameters r and s, which represent the ratios between dark energy and dark matter and the other cosmic fluid respectively, are analyzed in terms of the stability of stationary solutions. The obtained general results allow to shed some light on the equations of state of the three interacting fluids, due to the constraints imposed by the stability of the solutions. We found that for an interaction proportional to the sum of the dark energy density and the third fluid density, the hypothetical fluid must have positive pressure, which leads naturally to a cosmological scenario with radiation, unparticle or even some form of warm dark matter as the third interacting fluid.     

飞秒暗孤子间相互作用的数值研究

通过数值模拟对飞秒暗孤子间的相互作用进行了研究，并且同飞秒亮孤子和皮秒暗孤子分别进行了比较，结果表明：同飞秒亮孤子相比，飞秒暗孤子间的相互作用比较小，前者表现为相互吸引、碰撞、合二为一，然后相互排斥，不具有周期性；而后者从一开始就相互排斥，且这种排斥作用较亮孤子来说相当微弱，同样也不具有周期性。此外，数值模拟的结果还表明，飞秒暗孤子间的相互作用同皮秒尺度下暗孤子间的相互作用基本一致，并且通过计算表明，飞秒暗孤子间的相互作用在一定范围内仍可利用皮秒尺度下暗孤子间相互作用的经验公式。但是，数值模拟结果显示，两孤子的初始间距越小，由经验公式计算结果所带来的误差就越大。     

暗物质及暗物质粒子探测

文章首先对暗物质的概念作了简单介绍,接着介绍了暗物质的发现过程和暗物质存在的证据等.随后,介绍了目前人们对暗物质粒子基本性质的理解和目前比较流行的暗物质模型,并解释了弱相互作用重粒子(WIMP)为什么获得人们最多的关注.文中还简单介绍了目前探测暗物质粒子的三种实验方法:对撞机探测法、直接探测法和间接探测法.最后,介绍了目前暗物质探测的最新进展,包括来自DAMA,CoGent,PAMELA,ATIC,Fermi等实验的最新结果.